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"guide_fingerprint": "2d11688d5546039e5fb26a2896f2ac6b9e9b36331f03724ee52c4d784dcd08da" }, { "arxiv_id": "2610.12322", "revision": 1, "source_fingerprint": "73b8e0280105442b3e3eb4d62ce30fa5ce0666c263133ecff92f40e8f12961d6", "guide_fingerprint": "c63a990e41e3fd49d2ba99553bb260e19b2b663a71a6f6e90f9d7fbe5897b45f" }, { "arxiv_id": "2610.12323", "revision": 1, "source_fingerprint": "c0757715fe81eeebb8eecb3ab7d8a0559d52a74348c20c7b774b88a9c46c78c3", "guide_fingerprint": "ea55503bac4d5bc37eaa35bb6c154f31d441af16b425302586689bb3dabb6775" }, { "arxiv_id": "2610.12394", "revision": 1, "source_fingerprint": "9e6584e88d1070dc91237dceea3914bab297c7591cb435f70b6005422d487ee1", "guide_fingerprint": "f0d032b1b9a24aca403e2659a4ccb2bd95d2c590466a3092ec3644c9ff6fef06" }, { "arxiv_id": "2610.12429", "revision": 1, "source_fingerprint": "ab8f82e768acf1ec76ed81e8520cdeac8e68ea2ca9da4e2f74e0e75d4cd7663e", "guide_fingerprint": "4ade135ebc1c79c3f4ce73adeb2d8139bc5c66ddebcc25c57a0d9f7151a93dae" }, { "arxiv_id": "2610.12462", "revision": 1, "source_fingerprint": "8156b8ff8488bc9bd51e9c0345019cda133e5ded8e250ee33860b679bb8dbb64", "guide_fingerprint": "455c0b5f4fb8536dd77a08a62dcef30c55d25e004d921c4dbca1f6762628f082" } ], "worth_knowing_summary": "推导了日冕磁饱和半径 $r_c/r_g \\simeq (r_0/r_g) q_c^{1/(p-g)} \\sim 10\\,r_g$、内部饱和磁通标度 $B_r \\propto r^{-2}$ 及归一化磁通 $\\phi \\sim 50$（与 MAD 饱和平台相符）。；中微子味转化在 $\\bar{\\nu}_e$ 过剩的南极区域最为显著；味转化引起电子轻子数（ELN）单极矩 $n_{\\mathrm{ELN}}^{(0)}$ 出现净亏损，使外边界归一化 ELN 偶极矩 $d_{\\mathrm{ELN}} = n_{\\mathrm{ELN}}^{(1)} / n_{\\mathrm{ELN}}^{(0)}$ 在 $r \\gtrsim 30\\,\\mathrm{km}$ 处增强约 $5\\% \\text{--} 10\\%$，且该增强效应独立于中微子质量排序。 等。", "skim_summary": "Impact of site-dependent noise configurations on Einstein Telescope science at low frequency、Kinematic and Dynamical Properties of Solar Neighborhood White Dwarfs from SDSS DR19 and Gaia DR3 等主题。" }, "counts": { "total": 72, "analyzed": 72, "pending": 0, "must_read": 1, "worth_knowing": 12, "skip": 59 }, "groups": { "must_read": [ { "arxiv_id": "2610.12359", "revision": 1, "title": "Funnel Leakage of the Wien Fireball in the Early Nebula after a Binary Neutron Star Merger", "abstract": "A newborn neutron star (NS) that survives after a binary NS merger can inject its rotational energy into the surrounding ejecta while the ejecta are still optically thick. The injected energy is redistributed by the pair cascade, and the nebula becomes a radiation-dominated plasma composed of photons and e^+- pairs. Compton scattering then governs the energy exchange while the photon number is conserved in scattering. This nebula is evolved with a one-zone model that includes pair creation, annihilation, photon injection, diffusion, and in particular the leakage through the jet-induced polar funnel. For typical parameters, we find that the Compton parameter y is much larger than unity at early times. The nebula therefore remains in saturated Comptonization for 100 s to a few thousand seconds, depending on the magnetic field strength of the post-merger NS. The radiation field takes a Wien spectrum with a Compton equilibrium temperature. The nebula is then a so-called Wien fireball. The Compton temperature decreases from tens of keV to a few keV at early times. As long as the ejecta are optically thick, the funnel leakage is comparable to or exceeds the adiabatic loss. The funnel emission is quasi-thermal, and its isotropic-equivalent luminosity is much higher than the spin-down luminosity. We suggest that the quasi-thermal components observed in the extended emission of short gamma-ray bursts could come from the funnel leakage of the nebula fireball.", "published": "2026-10-08T17:23:48Z", "updated": "2026-10-08T17:23:48Z", "authors": [ "Shao-Ze Li", "Yun-Wei Yu", "He Gao", "Peng-Cheng Yang", "Yu Qu" ], "url": "https://arxiv.org/abs/2610.12359v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12359", "revision": 1, "status": "ready", "source_fingerprint": "728a74ebc56c26b6be73b446e02eeaaa5f467775365b2832b08a5fa97c8b1f52", "priority": "must_read", "coverage": { "level": "full_body", "label": "已检查版本匹配的完整 TeX 正文", "source_version": "arXiv:2610.12359v1", "inspected_sections": [ "Introduction", "Funnel Leakage of the Wien Fireball in the Early Nebula after a Binary Neutron Star Merger", "I Introduction", "II Early Nebula Fireball", "III Fireball Evolution", "IV Funnel Leakage", "V Conclusion and Discussion", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12359v1", "locator": "Full body", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "181a0bedb2ec6bc3db49d01af3749ddd60d322cd2b4cfb6ed09272c03d6b3d4b" } ], "source_sections": [ "Introduction", "Funnel Leakage of the Wien Fireball in the Early Nebula after a Binary Neutron Star Merger", "I Introduction", "II Early Nebula Fireball", "III Fireball Evolution", "IV Funnel Leakage", "V Conclusion and Discussion", "References", "Instructions for reporting errors" ], "section_coverage": { "problem": true, "assumptions": false, "method": false, "results": false, "limitations": true, "appendices": "not_applicable" } }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:22:03.111Z", "reason": "本文建立了双中子星并合后新生毫秒磁星驱动早期星云火球在极区漏斗（polar funnel）中泄漏的解析与数值演化模型，完美连接了短 GRB 早期 X 射线延展辐射/平台期（准热 Wien 谱向非热谱转变）与千新星中心引擎供能过程，为高能瞬变源平台期辐射起源提供了核心动力学与辐射传输理论。", "result": "研究表明早期星云由饱和正负对级联主导，平衡态正负对数 $N_{\\pm}=\\left[16 Y L_{\\rm sd} V/(3\\sigma_T m_e c^3)\\right]^{1/2}$ 导致极高散射光学深度 $\\tau_{\\rm n} \\sim 10^3$，康普顿参数 $y \\gg 1$ 使辐射场演化为化学势 $\\mu_\\gamma < 0$ 的 Wien 火球（温度 $kT_{\\rm C} \\simeq \\Lambda kT_{\\bb} \\sim 10\\,\\mathrm{keV}$）。极区漏斗中的总泄漏光度 $L_{\\rm fun}=L_{\\rm fd}+L_{\\rm fo}$ 由相对论性对流外流占绝对主导（$L_{\\rm fo}/L_{\\rm fd} \\simeq \\zeta \\tau_{\\rm n} \\gg 1$）。观测等效各向同性光度达 $L_{\\rm ob,iso} \\simeq (1-\\eta)L_{\\rm fun}/f_{\\rm b}$，成功解释了持续数十至数百秒、温度 $kT \\sim 10\\text{--}100\\,\\mathrm{keV}$ 的短 GRB 延展辐射和 X 射线平台期准热谱特征。", "reading_entry": "IV Funnel Leakage", "problem": "双中子星并合后新生磁星注入的巨大自转能被光学厚的动力学抛射物包裹，传统球对称星云模型难以直接解释视线方向观测到的强 X 射线延展辐射与具有高准热温度（$10\\text{--}100\\,\\mathrm{keV}$）的光球辐射特征，亟需厘清非球对称极区漏斗几何对饱和 Wien 火球演化、膨胀做功及辐射泄漏的调控机制。", "method": "结合磁星偶极辐射注入 $L_{\\rm sd}(t)=L_0(1+t/t_{\\rm sd})^{-2}$，建立耦合正负对产生-湮灭平衡、光子数平衡与星云做功的能量演化方程：$$\\frac{dE}{dt}=L_{\\rm sd}-(1-f_{\\rm b})\\left(P\\frac{dV}{dt}+L_{\\rm e}\\right)-L_{\\rm fun}$$并将漏斗泄漏分为光子扩散 $L_{\\rm fd}=f_{\\rm b}E/t_{{\\rm d},{\\rm n}}$ 和声速阻滞对流外流 $L_{\\rm fo}\\simeq \\zeta f_{\\rm b}(E/R)c$，系统求解火球能谱从饱和康普顿化 Wien 态到非热态的跃迁过程。", "assumptions": [ "双中子星并合后残余天体为强磁化毫秒磁星，且早期喷流在两极穿透抛射物形成几何张角为 $\\theta$（束缚因子 $f_{\\rm b}=1-\\cos\\theta$）的开放漏斗通道。", "早期抛射物和星云呈次相对论性膨胀，光子产生速率不足以实现完全黑体辐射，康普顿化主导形成化学势 $\\mu_\\gamma < 0$ 的 Wien 谱。" ], "limits": [ "外流绝热加速效率 $\\eta$ 和漏斗张角演化简化为唯象参数，未包含三维相对论磁流体（RMHD）对漏斗边缘剪切混合过程的精细模拟。" ], "citation_leads": [ "II Early Nebula Fireball: “Equating the creation and annihilation rates gives the equilibrium pair number,”", "II Early Nebula Fireball: “The fully thermalized early nebula develops a Wien spectrum with $\\mu_{\\gamma}<0$ rather than a blackbody spectrum with $\\mu_{\\gamma}=0$”", "IV Funnel Leakage: “The funnel leakage consists of two parts. One is the diffusion and escape of photons through the nebula along the funnel. The other is the advective outflow of the $e^{\\pm}$–photon plasma along the funnel.”", "IV Funnel Leakage: “Part of the fireball leaks through the funnel instead of driving the expansion, so the volume grows more slowly, which keeps $y$ above unity for longer. The parameter $y$ remains above unity at early times for the three magnetic fields and”" ], "research_progress": "明确给出了饱和对等离子体 Wien 火球的定标关系 $kT_{\\rm C} \\simeq \\Lambda kT_{\\bb} \\propto L_{\\rm sd}^{1/4} v_{\\rm ej}^{-3/4} t^{-1/2}$，证明了漏斗泄漏能显著减缓火球膨胀做功，从而将高康普顿参数状态（$y > 1$）的维持时间延长多达 30%，阐明了短 GRB 延展辐射中硬 X 射线准热成分与平台期后转为非热幂律谱的统一物理演化图景。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } } ], "worth_knowing": [ { "arxiv_id": "2610.10681", "revision": 1, "title": "Wind-Fed Magnetic Flux and the Emergence of X-ray Coronae in Active Galactic Nuclei", "abstract": "We propose a scenario for the onset of radiatively efficient Active Galactic Nuclei (AGN) in which circumnuclear stellar and supernova-driven winds supply mass and partially ordered magnetic flux to a compact disk reservoir around a supermassive black hole. A coherent poloidal component surviving advection to small radii strengthens inward, lowering the gas plasma beta until mean Maxwell stresses overtake MRI turbulence, compress the disk vertically, and open a magnetically dominated wedge above it. Within a quasi-force-free description of this wedge, the field self-organizes toward a critical twist at which the net radial transport changes sign, defining a magnetic saturation radius $r_c\\sim10\\,r_g$. The magnetic squeezing of the disk fixes the pressure balance at the interface between the disk and wedge, confining the accumulated flux at $r_c$: flux advected toward this boundary is preferentially shed, fixing $B_r\\propto r^{-2}$ in the interior. From the field topology alone we then derive a normalized saturation flux $φ\\sim 50$, consistent with the MAD plateau of GRMHD simulations. The resulting compact, time-dependent saturation region is a natural candidate for the AGN X-ray corona, being collisionless, magnetized, and, at high compactness, plausibly pair-rich, with hadronic pair injection providing a conditional additional channel. Its size, variability, and spectral hardness are controlled by $r_c$, the compactness, and the magnetization. We connect these scalings to observed coronal sizes, variability, and the power partition between the corona and jet. We further propose that Little Red and Blue Dots could represent a disk-reservoir phase preceding luminous AGN activity.", "published": "2026-10-07T18:00:01Z", "updated": "2026-10-07T18:00:01Z", "authors": [ "Rostom Mbarek" ], "url": "https://arxiv.org/abs/2610.10681v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10681", "revision": 1, "status": "ready", "source_fingerprint": "8c107663f3746ffb635563a01cfd3500d20c692d80bc8f5d0aa22284ff3c0e9e", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10681v1", "inspected_sections": [ "Introduction", "From circumnuclear star formation to inner disk magnetization", "Wind delivery of mass and coherent flux", "Angular momentum transport of ordered fields", "Formation of the magnetically dominated wedge", "Angular extent of the magnetically dominated wedge", "Disk squeezing from advected ordered fields", "Dynamics inside the magnetically dominated wedge", "Flux regulation and the magnetic saturation radius", "Twist-regulated forcing and stress saturation", "Existence and intermittency of saturation for different slopes", "Flux saturation for $rleq r_c$", "Polar force structure", "Normalized flux and confinement at $r_c$", "Synthesis and connection to MAD phenomenology", "Observable consequences", "The flux-saturated inner bundle as an X-ray corona", "Flux saturation and general coronal constraints", "Flux shedding as the driver of coronal turbulence", "Threshold coronal magnetization", "Characteristic and maximum coronal magnetization", "The X-ray luminosity of the corona", "$lx/lbol$ is independent of black-hole mass", "Kinetic competition: heating, escape, and radiative cooling", "Coronal magnetic field", "Variability timescales", "Hadron-driven pair loading and compactness regulation", "Flux-shedding power and coronal outflows", "Jet--corona power partition in flux-saturated states", "Why many radiative-mode systems remain weakly jetted", "Crossing into the radio-loud branch: spin, flux opening, and environment", "Synthesis", "Little Blue and Red Dots as candidate precursors to radiative-mode AGN", "Conclusions", "Acknowledgements", "Data Availability", "Radial Flux Bundle", "Column fraction above the wedge--disk interface", "Horizon cap on the twist $q_H$", "Intermediate value theorem and the existence of a magnetized bundle boundary", "Derivation of the polar EM force", "Derivation of the saturation flux $phi$", "Electromagnetic versus gravitational force", "Radiation-to-gas pressure ratio", "Radiation-supported wedge base", "Thin-disk thickness and cooling at $r_c$", "Location of the self-gravity boundary", "Comptonization in a collisionless plasma" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10681v1", "locator": "Introduction; From circumnuclear star formation to inner disk magnetization; Wind delivery of mass and coherent flux; Angular momentum transport of ordered fields; Formation of the magnetically dominated wedge; Angular extent of the magnetically dominated wedge; Disk squeezing from advected ordered fields; Dynamics inside the magnetically dominated wedge; Flux regulation and the magnetic saturation radius; Twist-regulated forcing and stress saturation; Existence and intermittency of saturation for different slopes; Flux saturation for $rleq r_c$; Polar force structure; Normalized flux and confinement at $r_c$; Synthesis and connection to MAD phenomenology; Observable consequences; The flux-saturated inner bundle as an X-ray corona; Flux saturation and general coronal constraints; Flux shedding as the driver of coronal turbulence; Threshold coronal magnetization; Characteristic and maximum coronal magnetization; The X-ray luminosity of the corona; $lx/lbol$ is independent of black-hole mass; Kinetic competition: heating, escape, and radiative cooling; Coronal magnetic field; Variability timescales; Hadron-driven pair loading and compactness regulation; Flux-shedding power and coronal outflows; Jet--corona power partition in flux-saturated states; Why many radiative-mode systems remain weakly jetted; Crossing into the radio-loud branch: spin, flux opening, and environment; Synthesis; Little Blue and Red Dots as candidate precursors to radiative-mode AGN; Conclusions; Acknowledgements; Data Availability; Radial Flux Bundle; Column fraction above the wedge--disk interface; Horizon cap on the twist $q_H$; Intermediate value theorem and the existence of a magnetized bundle boundary; Derivation of the polar EM force; Derivation of the saturation flux $phi$; Electromagnetic versus gravitational force; Radiation-to-gas pressure ratio; Radiation-supported wedge base; Thin-disk thickness and cooling at $r_c$; Location of the self-gravity boundary; Comptonization in a collisionless plasma", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "a7c94a2b03596d9416525b56f7e631693090285d78dacb8f4bfb4a1acf30455a" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:04:06.320Z", "reason": "该工作建立了核周星暴风输送有序磁通量至辐射高效吸积盘、并在此基础上自洽形成致密 X 射线日冕（$r_c \\sim 10\\,r_g$）与解释喷流-日冕功率分配的完整解析理论，对理解高能致密天体吸积物理、黑洞日冕形成及射电宁静/射电噪转变具有参考价值。", "result": "推导了日冕磁饱和半径 $r_c/r_g \\simeq (r_0/r_g) q_c^{1/(p-g)} \\sim 10\\,r_g$、内部饱和磁通标度 $B_r \\propto r^{-2}$ 及归一化磁通 $\\phi \\sim 50$（与 MAD 饱和平台相符）。给出日冕 X 射线光度标度律 $\\frac{L_X}{\\dot M_c c^2} \\simeq \\frac{\\mathcal{A}_X\\phi^2(1+q_c^2)}{8\\pi^2\\kappa_{\\rm x}}\\left(\\frac{r_c}{r_g}\\right)^{-2}$，证明 $L_X/L_{\\rm bol}$ 主要取决于载入日冕的质量流比例 $\\dot M_c/\\dot M_{\\rm tot}$，与黑洞质量 $M_\\bullet$ 无显式依赖。", "reading_entry": "The flux-saturated inner bundle as an X-ray corona", "problem": "在辐射高效吸积模式（radiative-mode）AGN 中，标准吸积盘如何在缺乏大尺度几何粗盘拖曳的情况下，向内平流足够强的极向磁通以形成小尺度致密硬 X 射线日冕并维持日冕动力学平衡。", "method": "结合核周恒星形成风的磁通弹道捕获模型、吸积盘内外应力（平均麦克斯韦应力与 MRI 湍流）转换准则，建立准无力场近似下的磁化楔形体动力学方程，求解径向有效电磁力 $f_r$ 与极向力 $f_\\theta$ 的力平衡条件及临界磁扭缠度 $q_c$。", "assumptions": [], "limits": [], "citation_leads": [ "$lx/lbol$ is independent of black-hole mass: “At fixed magnetic-bundle topology, the X-ray fraction is controlled by the loaded fraction $\\dot M_c/\\dot M_{\\rm tot}$ of the bulk inflow that enters the magnetized coronal phase, not by $M_\\bullet$.”" ], "research_progress": "将星暴风磁通供给、吸积盘垂直挤压、MAD 类似磁通饱和半径自调节（$r_c \\sim 10\\,r_g$）与 X 射线日冕的产生机制自洽统一，自然解释了 AGN 日冕 $L_X/L_{\\rm bol}$ 对 $M_\\bullet$ 的弱依赖性及大多数系统呈现弱喷流/射电宁静的物理根源。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10685", "revision": 1, "title": "Neutrino flavor conversion alters the lepton-emission self-sustained asymmetry in core-collapse supernovae", "abstract": "We solve the neutrino equations of motion in a half annulus, accounting for two spatial dimensions. At any location in the annulus, the neutrino momentum is characterized by a polar-angle distribution, two effective azimuthal angles, and an energy distribution. We explore how neutrinos change their flavor while decoupling from matter in the presence of the neutrino-driven hydrodynamical instability LESA (i.e., the Lepton-number Emission Self-sustained Asymmetry) during the stalled-shock phase of a core-collapse supernova. In our setup, LESA is responsible for an excess of $ν_e$'s ($\\barν_e$'s) in the Northern (Southern) region of the annulus. Crossings in the $ν_e$-$\\barν_e$ angular distributions appear in the ELN-depleted Southern region of the annulus, while crossings in the energy distributions of $ν_e$-$ν_x$ and $\\barν_e$-$\\barν_x$ are present throughout the annulus. We find that collisional instabilities drive flavor conversion just before neutrino decoupling, fast instabilities are prominent in the Southern region of the annulus, and slow instabilities dominate otherwise. Flavor conversion is most efficient in the Southern region and is responsible for a $5$-$10\\%$ enhancement of the LESA dipole, independent of the neutrino-mass ordering. Our findings suggest that direction-dependent flavor conversion can have implications for the development of global neutrino asymmetries and hydrodynamical instabilities in core-collapse supernovae.", "published": "2026-10-07T18:00:02Z", "updated": "2026-10-07T18:00:02Z", "authors": [ "Noah Roux", "Irene Tamborra", "Maryna Mesiura" ], "url": "https://arxiv.org/abs/2610.10685v1", "categories": [ "astro-ph.HE", "hep-ph" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10685", "revision": 1, "status": "ready", "source_fingerprint": "488bd116437fb68fbd06ac1d0d1b7b8a1fce0e9249a40997dede3d28c08c5d8d", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10685v1", "inspected_sections": [ "Introduction", "Neutrino flavor conversion alters the lepton-emission self-sustained asymmetry in core-collapse supernovae", "I Introduction", "II Equations of motion", "III Model setup", "III.1 FOCACCIA simulation setup", "III.2 LESA dipole", "IV Neutrino properties in the absence of flavor conversion", "V Linear stability analysis", "V.1 Discretized eigenvalue problem", "V.2 Growth rates: self-interaction Hamiltonian without attenuation", "V.3 Growth rates: self-interaction Hamiltonian with attenuation", "V.4 Dependence of the growth rate on the azimuthal angle in the momentum distribution", "V.5 Dependence of the growth rate on the neutrino mass ordering", "VI Flavor evolution in multiple spatial and momentum dimensions", "VI.1 Quasi-steady state flavor configuration", "VI.2 Angular and spectral distributions of neutrinos and antineutrinos", "VI.3 Impact of the attenuation of the self-interaction Hamiltonian", "VII Impact of flavor conversion on LESA", "VIII Discussion and conclusions", "Acknowledgements", "Appendix A Collisional rates", "A.1 Beta processes", "A.2 Pair processes", "A.3 Bremsstrahlung", "A.4 Neutral current scattering off nucleons", "A.5 Comparison among the reaction rates", "A.6 Comparison of our neutrino emission properties with the output of the benchmark supernova model", "Appendix B Numerical convergence tests", "B.1 Radial resolution", "B.2 Neutrino momentum polar angle resolution", "Appendix C Comparison between the quasi-steady state flavor configurations obtained in one- and two-spatial dimensions", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10685v1", "locator": "Introduction; Neutrino flavor conversion alters the lepton-emission self-sustained asymmetry in core-collapse supernovae; I Introduction; II Equations of motion; III Model setup; III.1 FOCACCIA simulation setup; III.2 LESA dipole; IV Neutrino properties in the absence of flavor conversion; V Linear stability analysis; V.1 Discretized eigenvalue problem; V.2 Growth rates: self-interaction Hamiltonian without attenuation; V.3 Growth rates: self-interaction Hamiltonian with attenuation; V.4 Dependence of the growth rate on the azimuthal angle in the momentum distribution; V.5 Dependence of the growth rate on the neutrino mass ordering; VI Flavor evolution in multiple spatial and momentum dimensions; VI.1 Quasi-steady state flavor configuration; VI.2 Angular and spectral distributions of neutrinos and antineutrinos; VI.3 Impact of the attenuation of the self-interaction Hamiltonian; VII Impact of flavor conversion on LESA; VIII Discussion and conclusions; Acknowledgements; Appendix A Collisional rates; A.1 Beta processes; A.2 Pair processes; A.3 Bremsstrahlung; A.4 Neutral current scattering off nucleons; A.5 Comparison among the reaction rates; A.6 Comparison of our neutrino emission properties with the output of the benchmark supernova model; Appendix B Numerical convergence tests; B.1 Radial resolution; B.2 Neutrino momentum polar angle resolution; Appendix C Comparison between the quasi-steady state flavor configurations obtained in one- and two-spatial dimensions; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "780fccd968eb2bdcdbd75f4306b64edea430fa923331ceab2b9ed058b5c4a36d" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:26:51.819Z", "reason": "论文研究核心坍缩超新星（CCSN）中心引擎中的中微子量子动理学输运，探讨味转化对大尺度轻子发射自持不对称性（LESA）的反馈效应，与超新星中心引擎及中微子物理研究兴趣直接相关。", "result": "中微子味转化在 $\\bar{\\nu}_e$ 过剩的南极区域最为显著；味转化引起电子轻子数（ELN）单极矩 $n_{\\mathrm{ELN}}^{(0)}$ 出现净亏损，使外边界归一化 ELN 偶极矩 $d_{\\mathrm{ELN}} = n_{\\mathrm{ELN}}^{(1)} / n_{\\mathrm{ELN}}^{(0)}$ 在 $r \\gtrsim 30\\,\\mathrm{km}$ 处增强约 $5\\% \\text{--} 10\\%$，且该增强效应独立于中微子质量排序。", "reading_entry": "VII Impact of flavor conversion on LESA", "problem": "在核心坍缩超新星吸积与激波停滞阶段，快味与碰撞中微子味转化是否以及如何在多维空间中影响自持轻子发射不对称性（LESA 偶极度）。", "method": "利用 GPU 加速代码 FOCACCIA 在二维半环形几何（$r, \\Theta$）与多维动量空间（$E, \\theta, \\phi$）求解有效双味中微子量子动理学方程：$i\\left(\\partial_t + \\mathbf{v}\\cdot\\mathbf{\\nabla}_{\\mathbf{r}}\\right)\\varrho = [\\mathcal{H}, \\varrho] + i\\mathcal{C}[\\varrho]$，结合局域线性稳定性分析（LSA）色散关系，并在深层区域采用哈密顿量衰减参数 $\\zeta_0$ 抑制计算开销。", "assumptions": [ "采用有效双味体系（$\\nu_e, \\nu_x$）进行近似" ], "limits": [ "忽略了非弹性中微子-电子及中微子-核子散射引起的能谱连续热化" ], "citation_leads": [ "Neutrino flavor conversion alters the lepton-emission self-sustained asymmetry in core-collapse supernovae: “Neutrino flavor conversion alters the lepton-emission self-sustained asymmetry in core-collapse supernovae”", "VII Impact of flavor conversion on LESA: “VII Impact of flavor conversion on LESA”", "II Equations of motion: “II Equations of motion”", "VI.3 Impact of the attenuation of the self-interaction Hamiltonian: “Impact of the attenuation of the self-interaction Hamiltonian”" ], "research_progress": "首次在多维几何与多动量维度下自洽求解含碰撞项的中微子量子动理学演化，证实中微子味转化会加强超新星的 LESA 偶极不对称性（提升约 $5\\% \\text{--} 10\\%$），而非抹平该宏观不对称。", "figures": [ { "url": "/arxiv-figures/2610.10685/fig5.png", "caption": "Figure 5: ELN–XLN angular distributions integrated over energy and in the plane spanned by cos ⁡ θ \\cos\\theta and radius for Θ = 0 \\Theta=0 (left), Θ = π / 2 \\Theta=\\pi/2 (middle) and Θ = π \\Theta=\\pi (right) in the absence of flavor conversion (top, w/o FC) and averaged between t sim = 275 ​ μ ​ s t_{\\mathrm{sim}}=275\\,\\mu\\mathrm{s} and t sim = 300 ​ μ ​ s t_{\\mathrm{sim}}=300\\,\\mu\\mathrm{s} when the quasi-steady state flavor configuration has been reached in the presence of flavor conversion (bottom, w/ FC). Each panel displays the distributions for ϕ = 0 \\phi=0 (right half) and ϕ = π \\phi=\\pi (left half). The solid (dashed) horizontal line marks the ν e \\nu_{e} ( ν ¯ e \\bar{\\nu}_{e} ) decoupling radius. Without flavor conversion, ELN crossings are not present at Θ = 0 \\Theta=0 and π / 2 \\pi/2 , but appear at Θ = π \\Theta=\\pi (with XLN crossings not being present for any Θ \\Theta because ν x = ν ¯ x \\nu_{x}=\\bar{\\nu}_{x} ). Fast flavor conversion is responsible for erasing the ELN-XLN crossings at Θ = π \\Theta=\\pi .", "label": "Fig. 5", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true }, { "url": "/arxiv-figures/2610.10685/fig7.png", "caption": "Figure 7: Spectra of ν e \\nu_{e} – ν x \\nu_{x} ( ν ¯ e \\bar{\\nu}_{e} – ν ¯ x \\bar{\\nu}_{x} ) integrated over angle on the right (left) side of each plot in the plane spanned by the neutrino energy and the radius for Θ = 0 \\Theta=0 (left), Θ = π / 2 \\Theta=\\pi/2 (middle) and Θ = π \\Theta=\\pi (right) in the absence of flavor conversion (top, w/o FC) and averaged between t sim = 275 ​ μ ​ s t_{\\mathrm{sim}}=275\\,\\mu\\mathrm{s} and t sim = 300 ​ μ ​ s t_{\\mathrm{sim}}=300\\,\\mu\\mathrm{s} when a quasi-steady state configuration has been reached in the presence of flavor conversion (bottom, w/ FC). The black solid and dashed horizontal lines represent the electron neutrino and antineutrino decoupling radii, respectively. Black dotted and dot-dashed lines refer to the heavy-lepton flavor neutrino and antineutrino decoupling radii. The dot-dashed lines overlap with the dashed lines, except in the rightmost lower panel. Spectral crossings appear across the half annulus, even before neutrino decoupling.", "label": "Fig. 7", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10951", "revision": 1, "title": "Flux Dependence of the 1\\,keV Soft X-ray Feature in SAX J1808.4-3658 with \\textit{NICER}", "abstract": "We present a systematic X-ray spectral analysis of the 2019 and 2022 outbursts of the accreting millisecond pulsar SAX J1808.4-3658 with extit{NICER} with a particular emphasis on the nature of the longstanding $\\sim$1\\,keV spectral feature. We report here the first clear evidence that the 0.9-1.0 keV feature varies systematically with source brightness, exhibiting strong correlations with both continuum and blackbody flux. This establishes that the feature is directly coupled to the accretion process. The scaling and energy distribution of the feature differ between outbursts, corresponding to a $\\sim$2\\,dex change in reprocessor density (log\\,$n_e \\approx 19.1$ in 2019 vs. $\\sim$17.3 in 2022), which naturally explains the stronger, broader feature in 2019 and the weaker, more localized $\\sim$1\\,keV feature in 2022, in agreement with high-density reflection models. These results provide the strongest constraints to date on the origin of the $\\sim$1\\,keV feature in SAX J1808.4-3658.", "published": "2026-10-07T22:09:06Z", "updated": "2026-10-07T22:09:06Z", "authors": [ "Katherine Bruce", "Anne M. Lohfink", "Jaiverdhan Chauhan", "Suchismito Chattopadhyay", "Sachiko Tsuruta", "Andrew C. Liebmann" ], "url": "https://arxiv.org/abs/2610.10951v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10951", "revision": 1, "status": "ready", "source_fingerprint": "eaa02d5ffef98d5dc2a64178543bc68d41f3fe5478b00784dfe209266122ba64", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10951v1", "inspected_sections": [ "Introduction", "Observations and Data Reduction", "Results", "Continuum Modeling", "Soft Feature", "Discussion and Conclusions", "Acknowledgments" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10951v1", "locator": "Introduction; Observations and Data Reduction; Results; Continuum Modeling; Soft Feature; Discussion and Conclusions; Acknowledgments", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "6d911cc7a315965c6a2f724980abf0a1eb352988e1652c3234eba8dfba7f6348" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:07:10.576Z", "reason": "文章系统分析了著名吸积毫秒脉冲星 SAX J1808.4-3658 在 2019 与 2022 年爆发期间的 NICER 光谱，首次量化证实了 ~1 keV 软 X 射线超额发射与连续谱及黑体热点通量的正相关性，并基于高密度反射模型解释了谱特征的演化，为致密天体吸积物理与高能观测提供了观测约束。", "result": "在 0.9--1.0 keV 探测到的软 X 射线特征与源亮度紧密耦合：2019 年高斯线归一化与计数率 ($r=0.8^{+0.1}_{-0.3}$)、主连续谱通量 ($r=0.9\\pm0.1$)、黑体通量 ($r=0.8\\pm0.1$) 及反射通量 ($r=0.7^{+0.1}_{-0.2}$) 呈显著正相关；2022 年同样与连续谱 ($r=0.9\\pm0.1$) 和黑体通量 ($r=0.9\\pm0.1$) 强相关，但与反射通量相关性不显著 ($r=0.1^{+0.5}_{-0.6}$)。Deming 回归斜率从 2019 年的 $(4.0\\pm0.3)\\times10^{6}$（连续谱）和 $(7.3\\pm0.5)\\times10^{7}$（黑体）降至 2022 年的 $(1.8\\pm0.2)\\times10^{6}$ 和 $(3.3\\pm0.3)\\times10^{7}$。高斯线能量分布与强度的差异与再处理器电子数密度的变化一致（2019 年 $\\log (n_e/\\mathrm{cm^{-3}}) \\approx 19.1$，2022 年 $\\approx 17.3$）。", "reading_entry": "Discussion and Conclusions", "problem": "中子星低质量 X 射线双星及毫秒脉冲星长期存在 ~1 keV 软 X 射线超额辐射的起源争议，缺乏在完整爆发周期内检验该结构是否随吸积流量与辐射组分系统性演化的观测证据。", "method": "利用 HEASoft/NICERDAS 分析 2019 与 2022 年 81 组高质量 NICER 能谱（0.7--10.0 keV），以基线模型 \\texttt{TBfeo} $\\times$ (\\texttt{relxillCp} + \\texttt{bbodyrad}) 拟合连续谱，并以 0.1 keV 步长在 0.7--1.4 keV 网格搜索零线宽高斯成分（以 $\\Delta\\chi^2 \\ge 9$ 即 $3\\sigma$ 作为单次检测阈值）；通过 20,000 次 Monte Carlo 模拟评估各辐射组分通量与高斯线强度的 Pearson 相关系数及 Deming 回归斜率。", "assumptions": [ "除光子指数 $\\Gamma$、反射份额 $R_f$、黑体温度 $kT_{\\rm bb}$ 及各组分归一化外，其余参数固定为联合 NICER/NuSTAR 宽能带拟合结果。" ], "limits": [ "不能完全排除残余低能仪器校准不确定度对 1 keV 结构的影响。" ], "citation_leads": [ "Introduction: “A long‑standing question in accreting neutron‑star systems is the origin of a soft X‑ray excess near 1\\,keV.”", "Observations and Data Reduction: “Spectra were grouped to a minimum of 20 counts per bin to ensure the validity of $\\chi^{2}$ statistics in XSPEC.”", "Soft Feature: “A trial is counted as a detection if it improves the fit by $\\Delta\\chi^{2}\\!\\ge\\!9$ (corresponding to 3$\\sigma$ single-trial significance)”", "Soft Feature: “The Deming regression slopes show a much shallower relationship in 2022 compared to 2019, decreasing from $(4.0\\pm0.3)\\times10^{6}$ to $(1.8\\pm0.2)\\times10^{6}$ for the primary continuum”", "Continuum Modeling: “Only the photon index, reflection fraction, blackbody temperature, and component normalizations were allowed to vary during spectral modeling;”", "Discussion and Conclusions: “While we cannot completely exclude a contribution from residual calibration uncertainties, we consider an instrumental origin very unlikely.”", "Discussion and Conclusions: “In summary, the 1\\,keV feature in J1808 is recurrent and flux-dependent.”" ], "research_progress": "首次确立了 SAX J1808.4-3658 中 ~1 keV 特征发射随源亮度和黑体/连续谱通量的定量标度律，并指出电子密度变化（$\\Delta \\log n_e \\sim 2$）可自然解释不同爆发时期线轮廓与反射耦合强弱的演化。", "figures": [ { "url": "/arxiv-figures/2610.10951/paramplotdoublerev1.png", "caption": "Figure 1 : Evolution of SAX J1808.4 − - 3658 across the 2019 and 2022 outbursts as observed by NICER . Panels show (from top to bottom) the 0.7–10 keV count rate (per observation), the best fit χ 2 \\chi^{2} ,the best-fit continuum values for photon index ( Γ \\Gamma ), continuum normalization (N cont ), reflection fraction (R f ), blackbody temperature (kT BB ; keV), and blackbody normalization (N BB ) from the baseline model fitted without a Gaussian line at 1 keV ( TBfeo × \\times [ relxillCp + bbodyrad ]; see Section III ), and logarithmic reflection flux (log F R ; erg/cm 2 /s). Only the photon index, reflection fraction, blackbody temperature, and component normalizations were allowed to vary during spectral modeling; all other parameters were fixed to values adopted from Bruce et al. [8] (See Table 1 in Appendix A). The vertical dashed line marks the onset of the reflaring phase [ 3 , 32 ] . Colored markers indicate contemporaneous reference points from prior studies: green— Casten et al. [13] ; purple— Bruce et al. [8] ; red- Sharma et al. [51] ; orange— Bult et al. [9] . Spectra were grouped to a minimum of 20 counts per bin and fitted with χ 2 \\chi^{2} statistics (Section II )", "label": "Fig. 1", "category": "fitting", "category_badge": "数据拟合与模型对比", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11435", "revision": 1, "title": "Neutron star cooling with $Δ$ dUrca processes", "abstract": "The cooling of neutron stars (NSs) provides insight into their composition and equation of state. However, a complete understanding of this phenomenon is still an open question. The early stage of NS cooling is dominated by neutrino emission from the core, which rapidly cools the star. Urca processes are one such mechanism where neutrinos escape from the core, carrying away most of the heat. Nucleonic and hyperonic direct Urca processes are known rapid cooling mechanisms. The possible appearance of $Δ$ baryons in dense matter introduces additional weak-interaction channels, including $Δ$ direct Urca processes. Although such processes have been discussed in the context of $Δ$-admixed NS matter, their neutrino emissivities and impact on NS cooling have not been systematically investigated. In this work, for the first time we incorporate the neutrino emissivities of the relevant $Δ$ direct Urca processes into NS cooling simulations. We investigate the thermal evolution of $Δ$-admixed NSs and assess the impact of these additional neutrino emission channels on their cooling behavior. We find that $Δ$ direct Urca processes can provide an efficient neutrino-cooling mechanism and significantly accelerate the thermal evolution of NSs. Our results demonstrate that $Δ$ baryons and their associated weak-interaction processes can play an important role in explaining NSs with unusually low surface temperatures and provide a new connection between the composition of dense matter and NS cooling observations.", "published": "2026-10-08T07:57:57Z", "updated": "2026-10-08T07:57:57Z", "authors": [ "Yogeesh N", "Monika Sinha", "Vishal Parmar" ], "url": "https://arxiv.org/abs/2610.11435v1", "categories": [ "astro-ph.HE", "hep-ph" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11435", "revision": 1, "status": "ready", "source_fingerprint": "7704ecf5cf310ec1ad8a5e93488a632ed39f8ecb23c4b70b3618ab7272b4a041", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11435v1", "inspected_sections": [ "Introduction", "Neutron star cooling with $Delta$ dUrca processes", "1 Introduction", "2 NS cooling in presence of $Delta$ baryons", "2.1 Emissivity", "2.2 Implementation in NSCool", "3 Results", "3.1 Dependence on the meson–$Delta$ couplings", "3.2 Dependence on the envelope composition", "3.3 Implications for NS cooling", "4 Conclusions", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11435v1", "locator": "Introduction; Neutron star cooling with $Delta$ dUrca processes; 1 Introduction; 2 NS cooling in presence of $Delta$ baryons; 2.1 Emissivity; 2.2 Implementation in NSCool; 3 Results; 3.1 Dependence on the meson–$Delta$ couplings; 3.2 Dependence on the envelope composition; 3.3 Implications for NS cooling; 4 Conclusions; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "210c043df09e6d6fa31f1c6ebf56a09027a56274c9e88d8bdce0470d5683400a" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:23:05.964Z", "reason": "文章首次将 $\\Delta$ 重子直接 Urca（$\\Delta$ dUrca）弱相互作用通道的中微子发射率并入中子星热演化代码 NSCool，为致密天体热演化、高密核物质物态方程及年轻中子星的快速冷却观测特征提供了新的理论约束机制。", "result": "推导并应用了包含 $\\Delta^-$、$\\Delta^0$ 衰变的 $\\Delta$ dUrca 反应（$\\Delta^- \\rightarrow n+e^-+\\bar{\\nu}_e$、$\\Delta^- \\rightarrow \\Lambda+e^-+\\bar{\\nu}_e$、$\\Delta^0 \\rightarrow p+e^-+\\bar{\\nu}_e$）中微子发射率公式：$$Q = \\frac{457\\pi G_F^2 C^2}{3780\\,m_\\Delta^2 m_B^2}\\,T_9^6\\Big[(m_\\Delta^2-m_B^2)^2-2m_e^2(m_\\Delta^2+m_B^2)\\Big]\\left(f_1^2+3g_1^2\\right) m^*_\\Delta m^*_B m^*_e\\,\\Theta_{\\Delta Be}$$其中 $Q \\propto T_9^6$（$T_9 = T/10^9\\,\\mathrm{K}$）。在 DD-ME2 物态方程下，三类反应开启的临界重子数密度分别为 $3.35\\,n_0$、$3.55\\,n_0$ 和 $3.93\\,n_0$。该快速冷却过程显著加速高质量（$M \\simeq 1.8$–$1.9\\,M_\\odot$）中子星的冷却速率，可有效解释冷而年轻的孤立中子星表面温度观测。", "reading_entry": "2.1 Emissivity", "problem": "传统核子或奇异重子物质模型在解释部分年轻且表面温度极低的中子星观测时存在分歧，需明确超密核物质中引入 $\\Delta$ 重子后开启的额外直接 Urca 弱作用过程对中子星中微子发射率及长时标热演化曲线的具体影响。", "method": "基于 DD-ME2 参数化的相对论平均场（RMF）模型计算含 $\\Delta$ 与超子的物态方程，解析推导简并简并物质中 $\\Delta$ dUrca 过程的中微子发射率，并将其作为附加源项 $Q_\\nu^\\Delta$ 植入广义相对论一维热演化程序 NSCool 中，测试不同介子–$\\Delta$ 耦合参数、超流能隙及 Fe/H 包层模型对质量在 $1.4 \\le M/M_\\odot \\le 1.9$ 范围内中子星冷却轨线的影响。", "assumptions": [ "采用代表性的常数超流能隙 $\\Delta_{\\rm gap} = 1\\text{ MeV}$ 唯象描述密物质中 $\\Delta$ 重子的配对效应" ], "limits": [ "密物质中 $\\Delta$ 重子的有效配对能隙大小及其密度依赖性尚未完全确立，定量冷却曲线仍具有模型依赖性" ], "citation_leads": [ "Neutron star cooling with $Delta$ dUrca processes: “In this work, for the first time we incorporate the neutrino emissivities of the relevant $\\Delta$ direct Urca processes into NS cooling simulations. We investigate the thermal evolution of $\\Delta$-admixed NSs and assess the impact of”", "2.2 Implementation in NSCool: “NSCool includes a variety of standard neutrino-emission processes, such as the mUrca, dUrca, nucleon–nucleon bremsstrahlung, and Cooper-pair breaking and formation processes, together with the corresponding effects of baryon superfluidity.”", "4 Conclusions: “We have also investigated the effect of $\\Delta$ superfluidity. Since the $\\Delta$ pairing gap in dense matter is presently not well established, we have adopted a representative value of superfluid gap as 1 MeV.”" ], "research_progress": "首次在全相对论热演化模拟中完整定量计入 $\\Delta$ dUrca 过程（$Q \\propto T^6$），确认其在核心密度超过临界阈值（$n_b \\gtrsim 3.35\\,n_0$）的高质量中子星内部能触发类似标准核子 dUrca 的快冷却效应，且该增强冷却效应在不同包层组分与介子耦合参数变化下表现稳健。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11749", "revision": 1, "title": "A Coherent Harmonic Summing Pulsar Search Code", "abstract": "Pulsars have narrow pulses, so their signals spread over many harmonics in a Fourier transform. Standard pulsar searches add the powers of those harmonics and discard their phases, which throws away the pulse shape and some of the signal. Folding the time series at each trial period keeps both, but is expensive even with the Fast Folding Algorithm (FFA). We describe CoherentSearch.jl, an open-source Julia code that reconstructs the pulse profile at every trial spin frequency directly from the Fourier transform. It interpolates the complex amplitudes of typically 60 harmonics, inverse transforms them into a profile, and tests that profile against boxcar templates of many widths. Because the input spectrum is normalized, the noise in every profile is known in closed form, so one threshold gives one false-alarm rate across the whole search. In an injection study of over 860,000 simulated pulsars at a matched false-alarm rate, the new search recovers 76% of the pulsars in white noise, against 64% for riptide's FFA in its recommended configuration and 42% for PRESTO's accelsearch, and its threshold does not move under red noise. On one CPU core it is 1.4-2.2 times faster than riptide at matched frequency coverage, it scales to 27 times faster on 48 cores, and modern GPUs run it up to nine times faster than a 20-core workstation.", "published": "2026-10-08T11:40:09Z", "updated": "2026-10-08T11:40:09Z", "authors": [ "Scott M. Ransom" ], "url": "https://arxiv.org/abs/2610.11749v1", "categories": [ "astro-ph.IM", "astro-ph.HE" ], "primary_category": "astro-ph.IM", "analysis": { "arxiv_id": "2610.11749", "revision": 1, "status": "ready", "source_fingerprint": "3947d40793b2c08fc50be2caabeede924999fb1ec03b7fe26d31da3a35fda692", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11749v1", "inspected_sections": [ "Introduction", "A Coherent Harmonic Summing Pulsar Search Code", "I Introduction", "II The Coherent Search Algorithm", "II.1 The Algorithm in Pseudocode", "II.2 Code basics", "II.3 How many profile bins do we need?", "II.4 Preparing the input FFT", "II.5 Fourier Interpolation", "II.6 Harmonic Decimation", "II.7 Calculation of the search metric", "II.8 Other details", "III Comparisons with existing Search Codes", "III.1 Monte Carlo Simulations", "III.2 Results of the tests", "III.2.1 Sensitivity", "III.2.2 False-alarm rate", "III.2.3 Speed (single-threaded)", "III.2.4 Parallelism, and how real searches would be run", "III.2.5 Comparison with other papers comparing codes", "IV Conclusions", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11749v1", "locator": "Introduction; A Coherent Harmonic Summing Pulsar Search Code; I Introduction; II The Coherent Search Algorithm; II.1 The Algorithm in Pseudocode; II.2 Code basics; II.3 How many profile bins do we need?; II.4 Preparing the input FFT; II.5 Fourier Interpolation; II.6 Harmonic Decimation; II.7 Calculation of the search metric; II.8 Other details; III Comparisons with existing Search Codes; III.1 Monte Carlo Simulations; III.2 Results of the tests; III.2.1 Sensitivity; III.2.2 False-alarm rate; III.2.3 Speed (single-threaded); III.2.4 Parallelism, and how real searches would be run; III.2.5 Comparison with other papers comparing codes; IV Conclusions; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "8945a41f23e6183b7e47299831734a3ce1e153c16716d7d0f45f01b685a57dd2" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:32:01.814Z", "reason": "该工作提出了一种基于频域复振幅插值与相干反变换的脉冲星搜索新算法及开源代码 CoherentSearch.jl，在保持解析统计特性的同时兼顾了窄脉冲灵敏度与高计算效率。虽然属于射电脉冲星搜索方法学改进，未直接涉及 FRB/PRS 物理或高能爆发机制，但对脉冲星及致密天体周期性脉冲搜索（包括寻找双星脉冲星、磁星/中心引擎候选体）具有明确的研究工具价值。", "result": "提出了相干谐波求和脉冲星搜索算法，在傅里叶频率试探步长 $\\delta r = 1/(2H) = 1/n$ 下提取复振幅并重构 $n=2H$ 个相位元的脉冲轮廓，利用解析标准差 $\\sigma = \\sqrt{2 n_{\\rm low} + \\frac{1}{2} n_{\\rm nyq}}$ 计算盒式匹配滤波信噪比 $s = (S_w - \\delta S_{\\rm tot})/(\\sigma \\sqrt{w(1-\\delta)})$。在包含 869,574 颗模拟脉冲星的注入测试中，在固定虚警率（每观测 0.1 个）下该算法恢复率达到 76.3%，显著优于 rseek C（64.5%）和 accelsearch（41.6%），单线程计算速度较 fast folding 提升 1.7–7.3 倍，且 GPU 单卡耗时仅 $\\sim 4.3\\,\\mathrm{s}$。", "reading_entry": "II The Coherent Search Algorithm", "problem": "传统非相干谐波叠加（如 accelsearch）丢弃了傅里叶谐波的相位信息与脉冲轮廓形状，导致在窄占空比脉冲星搜索中灵敏度显著下降；而时域快速折叠算法（如基于 FFA 的 riptide）计算代价高昂且时域去红噪声滤波易导致虚警率漂移与浅折叠统计失真。", "method": "输入预处理采用白化傅里叶谱，使平均噪声功率归一化为 1；通过截断 Sinc 插值 $A_r \\simeq \\sum A_k \\mathrm{e}^{-\\mathrm{i}\\pi(r-k)} \\mathrm{sinc}[\\pi(r-k)]$（截断参数 $m=16$）提取基频及其 $H$ 个谐波的复振幅；利用谐波抽取（Harmonic Decimation，步长 $k$）以 $kr$ 频率同时覆盖更少谐波组合的高频自转；采用 Dirichlet 核解析计算带限滤波方差 ${\\rm var}(S_w)$，并利用前缀和与几何步长盒式滤波器进行候选体信噪比评估。", "assumptions": [], "limits": [ "默认配置（如 60 个谐波）在占空比极窄（$<0.5\\%$）时灵敏度稍低于超深阶梯 FFA 算法", "因各谐波与基频具有严格固定的频域比例关系，算法无法直接兼容傅里叶域频域加速度搜索（FDAS），必须依赖时域重采样实现轨道加速度补偿" ], "citation_leads": [ "II.1 The Algorithm in Pseudocode: “The algorithm in pseudocode”", "II.5 Fourier Interpolation: “Fourier Interpolation”", "II.6 Harmonic Decimation: “Harmonic Decimation”", "III Comparisons with existing Search Codes: “Comparisons with existing Search Codes”", "I Introduction: “Sensitivity”", "III.2.2 False-alarm rate: “False-alarm rate”", "III.2.4 Parallelism, and how real searches would be run: “Parallelism, and how real searches would be run”", "I Introduction: “Conclusions”" ], "research_progress": "建立了兼具非相干 FFT 搜索高速度与 FFA 算法高窄脉冲灵敏度的相干频域脉冲星搜索新范式，彻底消除了传统时域折叠的轮廓噪声估计偏差，且单次候选体列表缩小约一个数量级，支持 CPU 多核与 GPU 高度并行。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11813", "revision": 1, "title": "The Hand of God Revisited: Revealing the Shell Structure and Jet-Supernova Remnant Interaction in MSH 15-52", "abstract": "We present an X-ray analysis of the supernova remnant (SNR) MSH 15-52 associated with the young rotation-powered pulsar PSR B1509-58, using Chandra, XMM-Newton, and eROSITA, complemented by MeerKAT radio data. We report the discovery of the missing southern counterpart to the bright northern RCW 89 region and identify a foreground X-ray source that may be a previously unidentified SNR candidate. Imaging and spectroscopy with XMM-Newton and eROSITA reveal the shell properties of MSH 15-52 and suggest that both the southern and northern shell-like structures are consistent with shocked interstellar medium associated with the forward shock, while their low ionization timescales and possible hard power-law components indicate possible influence from particle injection or additional heating by the pulsar wind nebula (PWN) jets. New Chandra spectral maps of the southern jet reveal a region of hard non-thermal emission, with a photon index of approximately 1.6, suggesting interaction between the PWN and the reverse shock and possible re-acceleration of the pulsar outflow. Spatially resolved spectroscopy of the RCW 89 northern clumps reveals high-velocity, metal-rich ejecta with enhanced Ne and Mg abundances. Comparison with core-collapse nucleosynthesis models favors a massive progenitor with an initial mass of approximately 29 solar masses in one-dimensional yield models, while asymmetric explosion models show that lower-mass progenitors can also reproduce the observed abundance ratios. Our study supports a picture in which RCW 89 is part of a larger asymmetric SNR shell interacting with energetic pulsar jets, making the system a valuable laboratory for probing pulsar-PWN-SNR interaction.", "published": "2026-10-08T12:20:21Z", "updated": "2026-10-08T12:20:21Z", "authors": [ "Lingxiao Dang", "Isabel Sander", "Samar Safi-Harb", "Christopher Fryer" ], "url": "https://arxiv.org/abs/2610.11813v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11813", "revision": 1, "status": "ready", "source_fingerprint": "c03a191f56ddf2415d76f795558f5f12b028b5d80e18a7e624b659a9545a4728", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11813v1", "inspected_sections": [ "Introduction", "The Hand of God Revisited: Revealing the Shell Structure and Jet–Supernova Remnant Interaction in MSH 15–52", "I Introduction", "II Data", "II.1 Chandra", "II.2 XMM-Newton", "II.3 eROSITA", "III results", "III.1 The ejecta region", "III.2 The jet regions", "III.3 The shell region", "IV Discussion", "IV.1 Properties of the SNR", "IV.2 Properties of the PWN jets", "IV.3 Supernova Progenitor of MSH 15–52", "V Conclusions", "Acknowledgments", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11813v1", "locator": "Introduction; The Hand of God Revisited: Revealing the Shell Structure and Jet–Supernova Remnant Interaction in MSH 15–52; I Introduction; II Data; II.1 Chandra; II.2 XMM-Newton; II.3 eROSITA; III results; III.1 The ejecta region; III.2 The jet regions; III.3 The shell region; IV Discussion; IV.1 Properties of the SNR; IV.2 Properties of the PWN jets; IV.3 Supernova Progenitor of MSH 15–52; V Conclusions; Acknowledgments; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "275c01d17e44e73a76901bb5f03f77cb6f1c95727a086ee69ea6597cf8eeebd7" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:24:31.995Z", "reason": "该工作利用 eROSITA、Chandra 与 XMM-Newton 综合多能段 X 射线观测，厘清了著名复合型超新星遗迹 MSH 15–52（PSR B1509–58，“上帝之手”）的南北壳层激波物理性质，并揭示了 PWN 相对论喷流与 SNR 壳层/反向激波相互作用特征，对研究脉冲星风云动力学及致密天体高能喷流具有参考价值。", "result": "eROSITA 首次揭示出远超出以往估计的北向热壳层及南壳层。在双成分（vpshock + powerlaw）模型下，北、南壳层激波温度分别为 $kT = 1.98^{+2.13}_{-0.71}\\ \\mathrm{keV}$ 和 $0.73^{+0.21}_{-0.18}\\ \\mathrm{keV}$，激波速度 $v_s = \\sqrt{16kT / (3\\mu m_p)}$ 对应为 $1300\\pm700\\ \\mathrm{km\\ s^{-1}}$ 与 $800\\pm100\\ \\mathrm{km\\ s^{-1}}$，推导的环境密度分别为 $n_{\\rm H} = 0.95\\pm0.27\\ \\mathrm{cm^{-3}}$ 与 $0.74\\pm0.19\\ \\mathrm{cm^{-3}}$，爆炸能量达 $E_0 \\approx (2.9-3.4)\\times 10^{51}\\ \\mathrm{erg}$；Sedov 年龄（北侧 $4.6\\pm2.5\\ \\mathrm{kyr}$，南侧 $12.1\\pm1.7\\ \\mathrm{kyr}$）显著大于脉冲星特征年龄（$1.7\\ \\mathrm{kyr}$）。南喷流区发现光子指数硬化至 $\\Gamma \\sim 1.6$，与反向激波-PWN 碰撞特征时标 $t_{\\mathrm{col}}=1045\\,E_{51}^{-1/2}\\left(\\frac{M_{\\mathrm{ej}}}{M_{\\odot}}\\right)^{5/6}n_{0}^{-1/3}\\ \\mathrm{yr} \\sim 5.0-6.8\\ \\mathrm{kyr}$ 一致，表明喷流正在与反向激波相互作用。", "reading_entry": "IV.2 Properties of the PWN jets", "problem": "复合型 SNR MSH 15–52 中长期缺失与北侧 RCW 89 对应的南部对称壳层，前向激波真正范围未知，且脉冲星风云（PWN）相对论喷流如何与 SNR 反激波/壳层介质相互作用并注入相对论粒子存在观测争议。", "method": "利用 eROSITA 与 XMM-Newton 大视场数据提取弥散壳层光谱并结合 `vpshock` 加非热幂律模型拟合；利用 Chandra 2017–2018 年共 $184.59\\ \\mathrm{ks}$ 高分辨数据通过 `contbin` 划分喷流区域构建光子指数 $\\Gamma$ 空间谱图；通过 Ne、Mg 等离子体发射线等效宽度（EW）结合多普勒频移拟合（`vashift`）解算富金属抛射物团块的三维空间速度 $v_{\\rm 3D} = \\sqrt{v_{\\rm LOS}^2 + v_r^2 + v_t^2}$。", "assumptions": [], "limits": [], "citation_leads": [ "The Hand of God Revisited: Revealing the Shell Structure and Jet–Supernova Remnant Interaction in MSH 15–52: “suggest that both the southern and northern shell-like structures are consistent with shocked interstellar medium associated with the forward shock”", "III.1 The ejecta region: “Motivated by previous reports of high-velocity ejecta in RCW 89, we adopted an absorbed vpshock model convolved with vashift to account for possible Doppler shifts in the emitting plasma.”", "III.3 The shell region: “A notable finding from the eROSITA data is the clear detection of a shell-like thermal structure in the northern region. Its location lies significantly farther out than the blast-wave position inferred by [Borkowski et al. [8]]”", "IV.2 Properties of the PWN jets: “t_{\\mathrm{col}}=1045\\,E_{51}^{-1/2}\\left(\\frac{M_{\\mathrm{ej}}}{M_{\\odot}}\\right)^{5/6}n_{0}^{-1/3}\\ \\mathrm{yr}”", "V Conclusions: “In the southern jet, we present evidence for a hard photon index region ($\\Gamma$$\\sim$1.6) suggesting an interaction with the SNR reverse shock at this location.”" ], "research_progress": "利用 eROSITA 首次确凿探测到南北壳层前向激波的热辐射，将前向激波范围向外延展；在南向 PWN 喷流处直接给出了与反激波碰撞硬化（$\\Gamma \\sim 1.6$）的谱学证据，给出了碰撞时标定标关系 $t_{\\mathrm{col}}=1045\\,E_{51}^{-1/2}(M_{\\mathrm{ej}}/M_{\\odot})^{5/6}n_{0}^{-1/3}\\ \\mathrm{yr}$。", "figures": [ { "url": "/arxiv-figures/2610.11813/erositadr2.png", "caption": "Figure 10: Multi-wavelength image of the region surrounding MSH 15–52. Red: ASKAP image, green: eROSITA image, and white contours showing the MeerKAT data. The blue elliptical region highlights the foreground source.", "label": "Fig. 10", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false }, { "url": "/arxiv-figures/2610.11813/multiwaveimage.png", "caption": "Figure 13: Multi-wavelength image of MSH 15–52 (red: MeerKAT image, green: 500–2000 eV eROSITA image, blue: 3000–8000 eV Chandra image). Contour of H.E.S.S. 30 excess map shown in green polygon [ 1 ] . The blue cross indicates the centroid of the HESS γ \\gamma -ray emission, which was derived by fitting the HESS data with a Gaussian profile [ 1 ] . The magenta diamond indicates the position of the pulsar, PSR J1513–5908.", "label": "Fig. 13", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11881", "revision": 1, "title": "From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus~X-3", "abstract": "Recent LHAASO observations reveal ultrahigh-energy (UHE) gamma-ray emission from Cygnus~X-3 with evidence for orbital modulation, providing a rare opportunity to study particle acceleration and transport on binary scales. We develop a common binary--jet model that jointly explains the contemporaneous GeV--PeV spectra and orbital light curves. The GeV emission is produced by anisotropic inverse-Compton scattering of stellar photons by relativistic electrons, while multi-PeV protons escaping from the inner region produce TeV--PeV gamma rays through photohadronic and hadronuclear interactions. The GeV orbital modulation constrains the binary--jet geometry, allowing the UHE observations to probe the escaping proton population and its interaction with the circum-binary environment. We find that the UHE emission is strongly regulated by the accretion-driven wind structure. In the present state, a fast disk wind displaces much of the denser Wolf--Rayet (WR) wind from the escaping-proton trajectories, suppressing hadronuclear emission. Changes in the strength, collimation, or orientation of the disk wind can expose the escaping protons to a much denser WR wind and enhance the PeV gamma-ray luminosity by orders of magnitude. This provides a possible connection to the much brighter, though unconfirmed, PeV activity reported in the 1980s, and links UHE gamma-ray activity to the accretion and outflow state of the binary.", "published": "2026-10-08T12:52:42Z", "updated": "2026-10-08T12:52:42Z", "authors": [ "Su-Yu Wan", "Ruo-Yu Liu", "Xing-Fu Zhang", "Dmitriy Khangulyan" ], "url": "https://arxiv.org/abs/2610.11881v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11881", "revision": 1, "status": "ready", "source_fingerprint": "ca5dbbe36eec22680cda39e846e159a1956a8e884c22ae4276e718605e21177c", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11881v1", "inspected_sections": [ "Introduction", "From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus X-3", "References", "Appendix A Spectrum of escaping protons", "Appendix B Calculation details and model checks", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11881v1", "locator": "Introduction; From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus X-3; References; Appendix A Spectrum of escaping protons; Appendix B Calculation details and model checks; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "30e1810b19d68f63dde7173182ceb576efbb395fc68166e052115cc4761947ec" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:23:19.233Z", "reason": "该工作建立了统一的双星-喷流相互作用辐射模型，成功联合拟合了 Cygnus X-3 在 GeV（Fermi-LAT）与 TeV–PeV（LHAASO）波段的轨道调制光变及能谱，澄清了吸积盘风与伴星风动压平衡对超高能强子辐射效率的调节机制，对微类星体极端粒子加速与喷流物理具有直接参考价值。", "result": "通过联合拟合确定喷流速度 $\\beta_{\\rm j} = 0.603^{+0.076}_{-0.071}$、GeV 电子辐射特征高度 $H_{\\rm GeV} = 2.75^{+0.33}_{-0.60}\\times 10^{11}\\,{\\rm cm}$；逃逸质子在 $H_{\\rm esc} \\sim 3.0 \\times 10^{10}\\,{\\rm cm}$ 注入，其能谱指数为 $s_p = 2.461^{+0.213}_{-0.165}$，截断能量 $E^{\\prime}_{p,\\rm cut} = 108^{+440}_{-80}\\,{\\rm PeV}$；观测者系两支喷流逃逸质子总功率与随动系内禀功率满足关系 $L_{p} = \\Gamma_{\\rm j}^{2}L^{\\prime}_{p}$。快速吸积盘风排挤了密集的 WR 伴星风，将朝向观测者方向的逃逸质子 $pp$ 相互作用核子靶柱密度压低约 2 个数量级，从而自然解释了 UHE 能谱形态并自洽压低了过强的强子碰撞背景。", "reading_entry": "From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus X-3", "problem": "如何构建自洽的统一物理图像，同时解释 LHAASO 探测到的 Cygnus X-3 高达 $3.7\\,{\\rm PeV}$ 的超高能伽马射线轨道调制，以及 Fermi-LAT 观测到的 GeV 能谱与轨道相位光变矛盾。", "method": "结合喷流多波段轻子与强子模型：GeV 辐射归因于喷流相对论电子对外禀 WR 星光子的各向异性逆康普顿散射（EC）；多 PeV 质子从亚双星尺度喷流逃逸并在双星介质中经 $p\\gamma$（结合 SOPHIA++ 模拟并考虑恒星视大小与 $\\tau_{\\gamma\\gamma}$ 吸收）与 $pp$ 过程辐射 UHE 伽马光子；通过双星动压平衡解出超临界吸积盘风与 WR 星风相互作用的接触间断面，以核子密度剖面 $n_i(r_i)=\\dot{M}_i/(4\\pi r_i^2 v_i m_p)$ 计算质子-质子碰撞效率；随动系到观测者系逃逸质子注入率遵从变换 $Q_{p,\\xi}(E_{p},\\Omega)=\\Gamma_{\\rm j}\\delta_{\\xi}Q^{\\prime}_{p}\\left(\\frac{E_{p}}{\\delta_{\\xi}},\\Omega^{\\prime}\\right)$。", "assumptions": [ "在喷流随动系下逃逸质子能谱分布假定为各向同性，其注入归一化由随动系单侧喷流光度决定：$L^{\\prime}_{p}/2=\\int dE^{\\prime}_{p}\\,d\\Omega^{\\prime}\\,E^{\\prime}_{p}Q^{\\prime}_{p}(E^{\\prime}_{p},\\Omega^{\\prime})$。" ], "limits": [ "模型基于超临界吸积图像，假定大部分超出球化半径的吸积物质通过盘风被抛出，其几何采用简化双极或薄层接触间断面近似。" ], "citation_leads": [ "From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus X-3: “The GeV component is produced by anisotropic inverse-Compton scattering of stellar photons by relativistic electrons in the jet, while multi-PeV protons released from the inner region propagate through the binary and produce TeV–PeV gamma”", "From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus X-3: “The UHE gamma-ray luminosity is regulated by both the power of escaping protons and the efficiency with which that power is converted into gamma rays. In our model, the latter is strongly controlled by the circum-binary gas distribution.”", "Appendix A Spectrum of escaping protons: “The distribution is assumed to be isotropic, with its normalization determined by $L^{\\prime}_{p}/2=\\int dE^{\\prime}_{p}\\,d\\Omega^{\\prime}\\,E^{\\prime}_{p}Q^{\\prime}_{p}(E^{\\prime}_{p},\\Omega^{\\prime})$.”", "Appendix B Calculation details and model checks: “In the supercritical picture, most of the excess supply inside the spherization radius is expelled, so that”" ], "research_progress": "揭示了微类星体 UHE 伽马射线光度同时受到逃逸质子注入功率 $L_p$ 和双星周星气体分布所调控的辐射转换效率的双重制约；证明了纯 WR 星风模型虽可复现 $<1\\,{\\rm PeV}$ 通量但因缺乏盘风屏蔽而无法同时协调 GeV 轨道调制与 PeV 光谱特征。", "figures": [ { "url": "/arxiv-figures/2610.11881/sketch_copy.png", "caption": "Figure 1: Sketch of binary–jet geometry. GeV emission is produced at H GeV H_{\\rm GeV} , while high-energy protons are released at an effective height H esc H_{\\rm esc} and interact with stellar photons and circum-binary gas. The WR and disk winds are separated by a contact discontinuity.", "label": "Fig. 1", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12101", "revision": 1, "title": "An updated model of neutrino emission from proto-neutron stars", "abstract": "We present an improved parametric model for neutrino emission from core-collapse supernovae that directly connects neutrino luminosity and average energy to stellar properties during emission. Our model incorporates two critical physical processes: convection within the proto-neutron star and the evolution of the neutrinosphere radius during the early emission phase. Using simulated datasets of supernova neutrino events in the Super-Kamiokande detector, we assess the sensitivity to astrophysical properties in the event of a future detection. We show that the neutrino mass ordering plays a crucial role in determining which parameters can be constrained by the observed neutrino data.", "published": "2026-10-08T15:03:12Z", "updated": "2026-10-08T15:03:12Z", "authors": [ "Matteo Ballelli", "Federica Pompa", "Christoph Ternes", "Marco Drago", "Giulia Pagliaroli" ], "url": "https://arxiv.org/abs/2610.12101v1", "categories": [ "astro-ph.HE", "astro-ph.SR", "hep-ph" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12101", "revision": 1, "status": "ready", "source_fingerprint": "2808642708539eacd0ecd1f91d106df8efa4de081c8f17b17a0676cda470d6f5", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12101v1", "inspected_sections": [ "Introduction", "An updated model of neutrino emission from proto-neutron stars", "I Introduction", "II Supernova neutrino emission model", "II.1 Cooling phase", "II.2 Accretion phase", "II.3 The role of neutrino flavor conversions in the stellar matter", "III Comparison with numerical simulations", "IV Data analysis", "V Results and discussion", "VI Conclusions", "Acknowledgements", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12101v1", "locator": "Introduction; An updated model of neutrino emission from proto-neutron stars; I Introduction; II Supernova neutrino emission model; II.1 Cooling phase; II.2 Accretion phase; II.3 The role of neutrino flavor conversions in the stellar matter; III Comparison with numerical simulations; IV Data analysis; V Results and discussion; VI Conclusions; Acknowledgements; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "d0dc5c151424e29900d5d4cf07ecc2a4120df352ef27f5ccbc27089df7382ed8" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:23:25.528Z", "reason": "该工作构建了涵盖对流与中微子球半径动态演化的原初中子星（PNS）中微子辐射参数化模型，并给出了 Super-Kamiokande 探测器对银河系超新星爆发（10 kpc）参数重建的约束能力，直接关联超新星中心引擎与致密天体形成物理。", "result": "通过三维 FORNAX 模拟校准并利用 MCMC 分析假定 $D=10\\;{\\rm kpc}$ 的 $18\\,M_\\odot$ 超新星在 Super-Kamiokande（IBD 探测道）记录的信号：在倒序质量排序（IO）下，冷却相主导探测事件（约 4248 个事件），能够灵敏重建中微子球收缩参数（渐近半径 $R_f=22.0^{+0.6}_{-0.6}\\;{\\rm km}$、收缩时标 $\\tau_{\\rm R}=0.36^{+0.03}_{-0.03}\\;{\\rm s}$、收缩幅度 $\\delta R=1.8^{+0.1}_{-0.1}\\;{\\rm km}$）；在正序质量排序（NO）下，吸积相主导早期发射（前 $0.5\\;{\\rm s}$ 占约 70%，总事件约 5154 个），压制了收缩特征重建，仅能约束渐近半径 $R_f=15.2^{+0.3}_{-0.3}\\;{\\rm km}$，但可精确限定吸积特征（$T_a=2.23^{+0.02}_{-0.02}\\;{\\rm MeV}$，$M_a=0.19^{+0.01}_{-0.01}\\;M_\\odot$）。", "reading_entry": "II Supernova neutrino emission model", "problem": "既有原初中子星（PNS）解析/唯象中微子发射模型往往忽略 PNS 内部对流和早期中微子球物理半径的动力学收缩，导致对核塌缩超新星早期中微子光度、能谱演化及探测器参数反演精度的偏离。", "method": "模型引入含时中微子球半径 $R_c(t)=R_f[1+\\delta R\\exp(-t/\\tau_{\\rm R})]$，冷却相平均能量满足 $\\langle E_\\nu(t)\\rangle=3.15\\,T_c(t)$，在对流开始时标 $\\bar{t}$ 之前经历升温时延 $\\tau_{\\rm Tc}$，之后满足幂律-超指数降温 $T_c(t)\\propto t^{-\\alpha_c}\\exp[-(t/\\tau_c)^{n_c}]$；吸积相考虑正电子俘获，$\\langle E_\\nu(t)\\rangle\\simeq 5T_a(t)$ 并在 $t=\\tau_a$ 处平滑拼接；计入恒星物质中的 MSW 味转化（NO 下 $P_{ee}\\simeq 0.68$，IO 下 $P_{ee}\\simeq 0.02$），结合拓展无泊松似然函数 $\\mathcal{L}=\\exp\\left[-\\int R(t){\\rm d}t\\right]\\prod_{i=1}^{N_d}\\left[\\int R(t'_i,E_{e^+})G(E_{e^+},E_i){\\rm d}E_{e^+}\\right]$ 与 `emcee` 进行贝叶斯参数重建。", "assumptions": [], "limits": [], "citation_leads": [ "An updated model of neutrino emission from proto-neutron stars: “Our model incorporates two critical physical processes: convection within the proto-neutron star and the evolution of the neutrinosphere radius during the early emission phase.”", "II.1 Cooling phase: “The factor $\\delta R$ represents the fractional decrease of the radius from the initial value to the final one over the timescale $\\tau_{\\text{\\tiny R}}”", "V Results and discussion: “For $t<\\tau_{a}$, accretion dominates the emitted $\\bar{\\nu}_{e}$ flux and, consequently, the $\\bar{\\nu}_{e}$ flux reaching Earth for NO.”" ], "research_progress": "相较于传统的静态中微子球发射模型，该工作首次将 PNS 内部对流诱发的温升与中微子球动力学几何收缩 $R_c(t)$ 耦合进解析通量模型，定量给出了不同中微子质量排序（NO vs IO）对超新星吸积参数与中微子球几何收缩参数测量能力的系统差异。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12334", "revision": 1, "title": "Quantum Co-Design of Inhomogeneous Many-Body Neutrino Fast Flavor Transformation", "abstract": "Dense-neutrino flavor evolution is a quantum many-body problem whose fully correlated treatment becomes rapidly more expensive with increasing particle number and spatial structure. We develop a \\texttt{QCNO} quantum simulation code that maps a inhomogeneous forward-scattering neutrino Hamiltonian with advection and finite-range interactions to TEBD2 product-formula quantum circuits, and connects ideal many-body simulation, backend-aware execution, and fault-tolerant resource estimation within the same physical model. We reproduce the exact many-body evolution of the suppressed mean-field-like transverse fast flavor instability through $N=30$ and show that even a single open-boundary interaction generates Rënyi entanglement and non-stabilizer magic, although noisy backends still produce polarization RMSEs of order $0.1$--$0.3$. The restricted active interaction graph of this problem allows us to estimate the circuit depth and $T$ gate cost through $N=50$ for both NISQ and fault-tolerant approaches. The measured TEBD2 error in our fiducial ideal simulation of order $10^{-3}$ motivates a synthesis tolerance $\\varepsilon_{\\rm syn}\\sim10^{-7}$, corresponding to about $70$ $T$ gates per $R_Z$ rotation. The generated circuit contains $1.4\\times10^4$ $T$ gates per qubit for open boundaries (twice that for closed boundaries), requiring an application-level logical-$T$ error target of order $10^{-7}$ for early fault-tolerant architectures.", "published": "2026-10-08T17:12:10Z", "updated": "2026-10-08T17:12:10Z", "authors": [ "Zoha Laraib", "Sherwood Richers", "Alessandro Baroni", "Kathleen Hamilton", "In-Saeng Suh" ], "url": "https://arxiv.org/abs/2610.12334v1", "categories": [ "quant-ph", "astro-ph.HE" ], "primary_category": "quant-ph", "analysis": { "arxiv_id": "2610.12334", "revision": 1, "status": "ready", "source_fingerprint": "363c0d5875b5bd44db32b78cd06205f0baecc5ef0aa65827ee044af6d30d0db0", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12334v1", "inspected_sections": [ "Introduction", "Quantum Co-Design of Inhomogeneous Many-Body Neutrino Fast Flavor Transformation", "I QCNO Framework", "II Results", "II.1 Application co-design", "II.1.1 Inhomogeneous fast flavor instability across system size N", "II.1.2 Many-body entanglement and stabilizer Rényi magic", "II.2 Hardware Co-design", "II.2.1 Noise Sensitivity", "II.2.2 Architecture-dependent circuit scaling", "II.3 Fault-tolerant co-design", "II.3.1 Synthesis accuracy and non-Clifford cost", "II.3.2 Geometry-dependent accumulation of $T$-gate resources", "II.3.3 Implications for the NISQ-to-fault-tolerant transition", "III Conclusions", "IV Acknowledgments", "Appendix A QCNO physics validation tests", "A.1 Vacuum oscillations", "A.2 Many-body neutrino self-interactions", "A.3 Homogeneous mean-field fast flavor instability", "Appendix B Inhomogeneous FFI", "B.1 TEBD2 Product-formula timestep convergence", "B.2 Backend-based evolution under different geometries", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12334v1", "locator": "Introduction; Quantum Co-Design of Inhomogeneous Many-Body Neutrino Fast Flavor Transformation; I QCNO Framework; II Results; II.1 Application co-design; II.1.1 Inhomogeneous fast flavor instability across system size N; II.1.2 Many-body entanglement and stabilizer Rényi magic; II.2 Hardware Co-design; II.2.1 Noise Sensitivity; II.2.2 Architecture-dependent circuit scaling; II.3 Fault-tolerant co-design; II.3.1 Synthesis accuracy and non-Clifford cost; II.3.2 Geometry-dependent accumulation of $T$-gate resources; II.3.3 Implications for the NISQ-to-fault-tolerant transition; III Conclusions; IV Acknowledgments; Appendix A QCNO physics validation tests; A.1 Vacuum oscillations; A.2 Many-body neutrino self-interactions; A.3 Homogeneous mean-field fast flavor instability; Appendix B Inhomogeneous FFI; B.1 TEBD2 Product-formula timestep convergence; B.2 Backend-based evolution under different geometries; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "1d3fae755bc27af8558f2376adbfa0ad2bbd4abcf0fca2766805ffa7dd353bcc" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:52:44.345Z", "reason": "文章针对核心坍缩超新星爆发与中子星并合中的中微子快速味转换（FFI），构建了包含空间平流与非均匀相互作用的量子多体模拟框架（QCNO），揭示了许多体纠缠对传统平均场快速味不稳定性的压制效应，并定量评估了从 NISQ 硬件到容错量子计算（FTQC）的门开销标度律，对超新星中心引擎多体中微子集体效应的数值模拟方法具有参考价值。", "result": "通过对比平均场（MF）与许多体（MB）动力学发现：(1) 平均场横向相干度表现出指数型快速味失稳增长，增长率与解析值 $\\operatorname{Im}(\\Omega) = 2\\mu = 1.88\\times 10^{11}~\\mathrm{s}^{-1}$ 吻合；但在全关联许多体演化中（最高至体系尺寸 $N=30$），横向相干被显著压制在 $\\sim 10^{-10}$ 量级，纵向极化 $\\langle P_z \\rangle$ 去极化退相干至 0，并伴随第二 Rényi 熵 $S_2(\\rho_A) = -\\log_2 \\mathrm{Tr}(\\rho_A^2)$ 与稳定子 Rényi 幻度 $M_2(\\rho_A)$ 的快速激增；(2) 在 NISQ 硬件（IBM 超导与 IonQ 离子阱）上，受限相互作用使单 Trotter 步原生门呈 $\\mathcal{O}(N)$ 标度，但硬件噪声导致极化均方根误差高达 $\\epsilon(\\langle P_z \\rangle)_{\\mathrm{RMSE}} \\sim 0.1\\text{--}0.3$；(3) 容错量子计算中，将旋转合成误差与二阶乘积误差匹配需门合成容限 $\\varepsilon_{\\mathrm{syn}} \\sim 10^{-7}$（单 $R_Z$ 消耗约 70 个 $T$ 门），开放边界下每量子比特累积 $T$ 门需求在 $\\sim 1.4\\times 10^4$ 处饱和，对应单个 $T$ 门的逻辑错误率上限目标为 $p_T \\sim 10^{-7}$。", "reading_entry": "II.1.1 Inhomogeneous fast flavor instability across system size N", "problem": "在核心坍缩超新星与双中子星并合等致密天体环境中，中微子自散射引发的快速味转换（FFI）主导了轻子数输运与电子度 $Y_e$ 的演化。然而，传统平均场假设忽略了真实的多体量子纠缠，而经典数值模拟受限于许多体希尔伯特空间的指数爆炸，亟需评估量子模拟算法与实际硬件在处理包含非均匀空间平流的中微子多体问题时的可行性与资源瓶颈。", "method": "构建包含真空振荡与有限程局域自散射的非均匀哈密顿量：\n$$H = H_{\\mathrm{vac}} + H_{\\nu\\nu} = \\frac{1}{2}\\sum_{i}s_i\\omega_i\\,\\vec{B}\\cdot\\vec{\\sigma}_i + \\frac{\\mu}{2}\\sum_{i= 1 and 5% at SNR >= 2 (95% confidence). PG 1553+113 has the lowest false-alarm probability, 4.7% after trials. Stable year-scale modulation is uncommon, and no source is established as periodic. The framework distinguishes persistent, stationary modulation from coherent variability whose period may evolve or fluctuate, but not the physical mechanism. PG 1553+113 and B2 1215+30 are candidates for monitoring and continuous gravitational-wave searches, although their stability does not establish a binary origin.", "published": "2026-10-08T17:22:50Z", "updated": "2026-10-08T17:22:50Z", "authors": [ "Adithiya Dinesh", "Alberto Domínguez", "Alba Rico", "Pablo Peñil", "Marco Ajello", "Sara Buson" ], "url": "https://arxiv.org/abs/2610.12356v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12356", "revision": 1, "status": "ready", "source_fingerprint": "c3f24f1b34bb8153dee412c8e040cab98d173ee6c7442b73b7950d421144024a", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12356v1", "inspected_sections": [ "Introduction", "A morphological search for stable year-scale modulation in gamma-ray blazars", "1 Introduction", "2 Theoretical background", "2.1 Geometric modulation", "2.2 Plasma-driven modulation", "2.3 Observable properties of the physical scenarios", "3 Data and sample selection", "3.1 Blazar sample", "3.2 Gamma-ray light curves", "4 Methodology", "4.1 Light curve decomposition via singular spectrum analysis", "4.2 Weighted wavelet Z-transform analysis and ridge extraction", "4.2.1 Quasi-periodic oscillation frequency tracking", "4.2.2 Analysis safeguards", "4.3 Derivation of morphological parameters", "4.4 Uncertainty estimation via flux randomization", "4.5 Common quality selection", "4.6 From parent sample to QPO candidates", "4.7 Calibration of the morphological thresholds", "4.8 Validation of the classification scheme", "5 Results", "5.1 The mechanism map: coherence versus drift", "5.2 The persistence plane: observation baseline versus longevity", "5.3 The observed volatility regime", "5.4 Validation against red-noise artifacts", "5.5 Calibration: completeness, purity and measurement response", "5.6 Rank II: coherent, evolving modulation", "5.7 How common is stable year-scale modulation?", "5.8 Why the morphology is measured on the detrended light curve", "6 Physical interpretation and ranking of QPO candidates", "6.1 Hierarchy of emission mechanisms", "6.1.1 Rank I: stable clocks", "6.1.2 Rank II: coherent, evolving modulation", "6.1.3 Rank III: residual candidates", "6.2 Relation to significance-based periodicity searches", "6.3 Implications for SMBBH searches", "6.4 Morphological dependence on the central engine and jet structure", "6.5 Remaining degeneracies and limitations", "7 Broader applicability of the framework", "8 Summary and conclusions", "Data availability", "References", "Appendix A Technical details of the pipeline", "A.1 Selection of the oscillatory SSA mode", "A.2 Ridge tracking", "A.3 Local noise floor", "A.4 Conditioning of the flux-randomization intervals", "Appendix B Case studies at the classification boundary", "B.1 A strong modulation that fades: PKS 2155$-$304 (IIIσ)", "B.2 A coherent but intermittent modulation: 4C +47.08 (IIIΠ)", "B.3 A stable modulation beyond the ceiling: S5 1044+71 (IIIP)", "B.4 A long, weak modulation: Mkn 501 (IIIQ)", "Appendix C The rigidity parameter $k$", "Appendix D Atlas of Rank II", "Appendix E Spectroscopic redshift compilation", "Appendix F Extended catalog of QPO candidates", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12356v1", "locator": "Introduction; A morphological search for stable year-scale modulation in gamma-ray blazars; 1 Introduction; 2 Theoretical background; 2.1 Geometric modulation; 2.2 Plasma-driven modulation; 2.3 Observable properties of the physical scenarios; 3 Data and sample selection; 3.1 Blazar sample; 3.2 Gamma-ray light curves; 4 Methodology; 4.1 Light curve decomposition via singular spectrum analysis; 4.2 Weighted wavelet Z-transform analysis and ridge extraction; 4.2.1 Quasi-periodic oscillation frequency tracking; 4.2.2 Analysis safeguards; 4.3 Derivation of morphological parameters; 4.4 Uncertainty estimation via flux randomization; 4.5 Common quality selection; 4.6 From parent sample to QPO candidates; 4.7 Calibration of the morphological thresholds; 4.8 Validation of the classification scheme; 5 Results; 5.1 The mechanism map: coherence versus drift; 5.2 The persistence plane: observation baseline versus longevity; 5.3 The observed volatility regime; 5.4 Validation against red-noise artifacts; 5.5 Calibration: completeness, purity and measurement response; 5.6 Rank II: coherent, evolving modulation; 5.7 How common is stable year-scale modulation?; 5.8 Why the morphology is measured on the detrended light curve; 6 Physical interpretation and ranking of QPO candidates; 6.1 Hierarchy of emission mechanisms; 6.1.1 Rank I: stable clocks; 6.1.2 Rank II: coherent, evolving modulation; 6.1.3 Rank III: residual candidates; 6.2 Relation to significance-based periodicity searches; 6.3 Implications for SMBBH searches; 6.4 Morphological dependence on the central engine and jet structure; 6.5 Remaining degeneracies and limitations; 7 Broader applicability of the framework; 8 Summary and conclusions; Data availability; References; Appendix A Technical details of the pipeline; A.1 Selection of the oscillatory SSA mode; A.2 Ridge tracking; A.3 Local noise floor; A.4 Conditioning of the flux-randomization intervals; Appendix B Case studies at the classification boundary; B.1 A strong modulation that fades: PKS 2155$-$304 (IIIσ); B.2 A coherent but intermittent modulation: 4C +47.08 (IIIΠ); B.3 A stable modulation beyond the ceiling: S5 1044+71 (IIIP); B.4 A long, weak modulation: Mkn 501 (IIIQ); Appendix C The rigidity parameter $k$; Appendix D Atlas of Rank II; Appendix E Spectroscopic redshift compilation; Appendix F Extended catalog of QPO candidates; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "e9e9c5bbf0eff1a188618adbe9cea2c5b774e18cad012027d21b9ccf8b6b6612" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:42:37.571Z", "reason": "该研究利用 Fermi-LAT 长达 18.1 年的光变曲线，针对伽马射线耀变体中的年标度准周期振荡（QPO）建立了基于相干度、漂移率和波动度的形态学分类框架，系统区分了相对论喷流/超大质量双黑洞（SMBBH）几何调制与红噪声伪信号，并给出了稳态调制的统计发生率上限，对高能瞬变源中心引擎与相对论喷流动力学研究具有重要的参考价值与方法学借鉴意义。", "result": "在 120 条高质量伽马射线光变曲线中筛选出 97 个源，仅识别出 2 个高相干稳定候选体（Rank I：PG 1553+113，周期 $P_{\\mathrm{obs}} = 2.11 \\pm 0.01\\,\\mathrm{yr}$；B2 1215+30，周期 $P_{\\mathrm{obs}} = 2.89 \\pm 0.02\\,\\mathrm{yr}$）以及 6 个频率演化候选体（Rank II，包括 Mkn 421）。统计模拟表明纯红噪声产生 Rank I 的假阳性率为 $1.10\\%$（期望 $1.3$ 个，实际观测 $2$ 个，二项检验 $p = 0.38$），并未表现出显著超额；Rank II（期望 $2.7$ 个，实际 $6$ 个）呈边缘超额（$p = 0.055$）。在 $95\\%$ 置信度下，伽马射线耀变体中周期在 $1\\text{--}3\\,\\mathrm{yr}$ 且振幅 $\\mathrm{SNR} \\ge 1$ 的稳态准周期调制发生率上限被严格限制在 $\\le 7\\%$（$\\mathrm{SNR} \\ge 2$ 时 $\\le 5\\%$）。", "reading_entry": "5.7 How common is stable year-scale modulation?", "problem": "伽马射线耀变体中报道的年尺度周期信号常被红噪声随机涨落伪造，且传统基于周期显著性的检测方法采取“严格周期 vs 纯随机”的两分法，忽视了相干寿命、频率漂移与周期抖动等形态特征，难以厘清调制源自超大质量双黑洞（SMBBH）轨道衰减、喷流进动还是等离子体不稳定过程。", "method": "流水线采用奇异谱分析（SSA，窗口长度 $L \\approx 0.4 N$）去除长期趋势并自适应分离主导振荡模式，随后在去趋势光变曲线上使用加权小波 Z 变换（WWZ，Morlet 核衰减参数 $c = 0.0125$）在限制频带 $1\\,\\mathrm{yr} \\le P \\le 6\\,\\mathrm{yr}$ 内提取瞬时极值脊线；通过脊线量化循环加权相干度 $Q = \\int_{\\mathrm{active}} \\sqrt{S(t)/S_{\\mathrm{noise}}(P)}\\,\\mathrm{d}t/P(t)$、相对漂移率 $\\varepsilon$、周期波动度 $\\sigma_{\\ln P}$ 及剔除影响锥（COI）后的持续性 $\\Pi$；最后通过 $10^3$ 次通量随机化与 $10^4$ 条红噪声对数正态模拟标定物理分类边界（如 Rank I 阈值要求 $Q - \\Delta Q > 3$，$|\\varepsilon| + \\Delta\\varepsilon < 0.02\\,\\mathrm{yr}^{-1}$，$\\sigma_{\\ln P} + \\Delta\\sigma_{\\ln P} < 0.06$）。", "assumptions": [], "limits": [], "citation_leads": [ "6.3 Implications for SMBBH searches: “Implications for SMBBH searches”", "5.4 Validation against red-noise artifacts: “Validation against red-noise artifacts”", "4.1 Light curve decomposition via singular spectrum analysis: “Light curve decomposition via singular spectrum analysis”", "5.7 How common is stable year-scale modulation?: “How common is stable year-scale modulation?”", "6.1 Hierarchy of emission mechanisms: “Hierarchy of emission mechanisms”" ], "research_progress": "建立了首个耀变体伽马射线 QPO 的定量形态学分类与物理机制映射体系，消除了仅凭显著性搜索带来的高误报率，并将全天伽马射线耀变体中 1–3 年尺度稳定几何时钟的内秉发生率限制在 $\\le 7\\%$，为多信使引力波背景及喷流进动模型提供了明确的群体统计约束。", "figures": [ { "url": "/arxiv-figures/2610.12356/4FGL_J0538.8-4405_comps_2_3_wwz_ridge_fit.png", "caption": "Figure 16: Rank II sources, continued: PKS 0537 − - 441 (4FGL J0538.8 − - 4405; P obs = 2.68 P_{\\mathrm{obs}}=2.68 yr, ε = − 0.031 ​ yr − 1 \\varepsilon=-0.031\\,\\mathrm{yr}^{-1} ), PKS 1502+106 (4FGL J1504.4+1029; 2.46 2.46 yr, + 0.023 ​ yr − 1 +0.023\\,\\mathrm{yr}^{-1} , a borderline member) and Mkn 421 (4FGL J1104.4+3812; 2.63 2.63 yr, + 0.018 ​ yr − 1 +0.018\\,\\mathrm{yr}^{-1} with intermediate volatility). Panels as in Fig. 15 . Measured on the SSA reconstruction instead of the light curve, the modulation of PKS 1502+106 appears stationary ( ε = 0.006 ​ yr − 1 \\varepsilon=0.006\\,\\mathrm{yr}^{-1} ), the clearest illustration of the smoothing discussed in Sect. 5.8 .", "label": "Fig. 16", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true }, { "url": "/arxiv-figures/2610.12356/4FGL_J1555.7_1111_comps_1_2_wwz_ridge_fit.png", "caption": "Figure 3: WWZ ridge analysis of the detrended light curve of PG 1553+113 (Fig. 2 ). The color map is the WWZ power as a function of time and period. The gray shaded region is the cone of influence, where the finite length of the light curve distorts the transform; it is excluded from every ridge statistic. Red crosses mark the ridge points at which the modulation is detectable above the local noise floor (the active points of Sect. 4.3 ); they trace the instantaneous period and are the points from which the morphological parameters are computed.", "label": "Fig. 3", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12398", "revision": 1, "title": "ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological Simulations", "abstract": "JWST has revealed massive star clusters at $z\\gtrsim 6$, which provide promising environments for massive black hole (MBH) seed formation. We introduce a new MBH seeding model for cosmological simulations, physically motivated by the runaway collisions in star clusters. Subgrid star clusters are generated according to the local ISM and evolved through stellar evolution and two-body relaxation. The masses of MBH seeds formed through runaway collisions are determined by the properties of their host clusters, including the effects of metallicity-dependent stellar winds. We further follow tidal disruption events (TDEs) with the evolving clusters, which can be enhanced in MBH binaries, and account for gravitational-wave (GW) recoil following MBH mergers. We implement this model in a constrained simulation of a 5$σ$ overdense region, where seeds of $10^{3}-10^{5.6}\\,M_\\odot$ form in clusters with $10^{4}\\leq m_{\\rm SC}\\leq 10^{8}\\,M_\\odot$. Because both the seed abundance and mass are directly connected to the local environment, we have a more physical $M_{\\rm BH}\\!-\\!M_{\\rm galaxy}$ scaling for low-mass galaxies ($M_{\\rm galaxy}\\sim10^{6-9}\\,M_\\odot$), a regime poorly described by previous seeding models. Multiple MBHs are naturally allowed to form in-situ within individual halos, producing a spatially clustered population. This increases the MBH merger rate by $\\sim100$ relative to other seeding models, significantly enhancing the expected LISA event rate. TDEs can dominate the growth of $10^{3-4}\\,M_\\odot$ MBHs and produce luminous flares of $L_{\\rm peak}\\sim 10^{42-43}\\,{\\rm erg\\,s^{-1}}$, increasing the observability of low-mass seeds. This seeding prescription accelerates early MBH growth at $z\\gtrsim 8$, while subsequent self-regulated gas accretion drives the central MBH toward similar masses $\\sim10^{8.6}\\, M_\\odot$ by $z=6$ across different seeding models.", "published": "2026-10-08T17:41:37Z", "updated": "2026-10-08T17:41:37Z", "authors": [ "Yihao Zhou", "Tiziana Di Matteo", "Claire E. Williams", "Aklant Kumar Bhowmick", "Marta Reina-Campos", "Carl L. Rodriguez", "Elena González Prieto", "Laura Blecha", "Rupert Croft" ], "url": "https://arxiv.org/abs/2610.12398v1", "categories": [ "astro-ph.GA", "astro-ph.HE" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12398", "revision": 1, "status": "ready", "source_fingerprint": "92b875f39edb78e3a130402b3e206fb6d78246daf5ef1dda47b7fa0649a6e4a1", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12398v1", "inspected_sections": [ "Introduction", "ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological Simulations", "I Introduction", "II Method", "II.1 ASTRID galaxy formation model", "II.2 Star-Cluster-based MBH seeding model", "II.2.1 StarFOF", "II.2.2 Cluster Formation Efficiency", "II.2.3 Star Cluster Population", "II.2.4 MBH Seeds in Star Clusters", "II.2.5 Star Cluster Evolution", "II.2.6 TDEs in Star Clusters", "II.2.7 Gravitational Wave Recoil", "II.3 Halo-based and Gas-based MBH Seeding Models", "III Simulation Setup", "IV Results", "IV.1 StarFOF Catalog", "IV.2 Star Cluster Populations", "IV.3 MBH Seeds Formed in Star Clusters", "IV.4 MBHs Population from Different Seeding Models", "IV.5 MBH-Galaxy Relation and Occupation Fraction", "IV.6 Mass Evolution of the Central MBH", "IV.7 Influence of GW Recoil", "IV.8 TDE Contribution to MBH Early Growth", "V Conclusion", "Acknowledgments", "Appendix A The linking length $ellstar$ for StarFOF catalogs", "Appendix B The $Mrm seed,min$ in star-cluster-based seeding model", "Appendix C Validation of the Constrained Realization", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12398v1", "locator": "Introduction; ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological Simulations; I Introduction; II Method; II.1 ASTRID galaxy formation model; II.2 Star-Cluster-based MBH seeding model; II.2.1 StarFOF; II.2.2 Cluster Formation Efficiency; II.2.3 Star Cluster Population; II.2.4 MBH Seeds in Star Clusters; II.2.5 Star Cluster Evolution; II.2.6 TDEs in Star Clusters; II.2.7 Gravitational Wave Recoil; II.3 Halo-based and Gas-based MBH Seeding Models; III Simulation Setup; IV Results; IV.1 StarFOF Catalog; IV.2 Star Cluster Populations; IV.3 MBH Seeds Formed in Star Clusters; IV.4 MBHs Population from Different Seeding Models; IV.5 MBH-Galaxy Relation and Occupation Fraction; IV.6 Mass Evolution of the Central MBH; IV.7 Influence of GW Recoil; IV.8 TDE Contribution to MBH Early Growth; V Conclusion; Acknowledgments; Appendix A The linking length $ellstar$ for StarFOF catalogs; Appendix B The $Mrm seed,min$ in star-cluster-based seeding model; Appendix C Validation of the Constrained Realization; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "8c39e53d7aef152c97a6ec8590b78811800fae9b79163c1fb47e7e3f40d1ed19" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:44:13.890Z", "reason": "本文在宇宙学模拟中建立了基于致密星团内失控恒星碰撞的大质量黑洞（MBH）种子生成、星团演化、引力波反冲及潮汐瓦解事件（TDE）驱动早期增长的亚网格物理模型。虽非研究组核心的 FRB/超新星激波破越，但所涉及的 TDE 爆发光度标度律、吸积模型与致密天体高能瞬变观测紧密相关，对高能天体物理背景具有参考价值。", "result": "在 $z=6$ 时，对于低质量种子（$M_{\\rm BH} \\le 10^4\\,M_\\odot$），TDE 驱动的质量增长率 $\\dot{M}_{\\rm TDE}$ 显著超越气体吸积率 $\\dot{M}_{\\rm gas}$ 并可达超爱丁顿水平；利用经验标度律 $\\log_{10}(L_{\\rm peak}/{\\rm erg\\,s^{-1}}) = \\alpha + \\beta \\log_{10}(M_{\\rm BH}/10^6\\,M_\\odot)$（$\\alpha=43.7\\pm0.1$, $\\beta=0.4\\pm0.1$），对于 $M_{\\rm BH} \\sim 10^3 - 10^5\\,M_\\odot$，TDE 爆发峰值光度可达 $L_{\\rm peak} \\sim 3\\times 10^{42} - 2\\times 10^{43}\\,{\\rm erg\\,s^{-1}}$，大幅提升了早期暗弱黑洞种子的瞬态可观测性。", "reading_entry": "II Method", "problem": "现有宇宙学模拟常依赖经验性的基于暗物质晕或冷气体的单一 MBH 播种处方，忽略了在致密星团等微观物理环境中失控碰撞成种、星团动力学演化及潮汐瓦解事件（TDE）对早期黑洞生长与瞬变辐射的贡献。", "method": "基于 ASTRID 宇宙学流体动力学框架，利用 StarFOF 结构结合星团形成效率 $\\Gamma$ 采样初始星团族；通过失控碰撞方程 $\\frac{\\mathrm{d}M_{\\mathrm{VMS}}}{\\mathrm{d}t}=(1-f_{\\mathrm{ml}})(\\dot{M}_{\\mathrm{df}}-\\dot{M}_{\\mathrm{dep}}-\\dot{M}_{\\mathrm{bin}})-\\dot{M}_{\\mathrm{wind}}$（其中 $\\dot{M}_{\\rm wind}\\propto M_{\\rm VMS}^{2.1}Z_{\\rm SC}^{0.74}$）计算超大质量恒星（VMS）质量并坍缩为种子（$M_{\\rm seed,min} = 10^3\\,h^{-1}M_\\odot$）；协同追踪星团两体弛豫质量损失、引力波反冲剔除以及包含单黑洞与双黑洞偏心 Kozai-Lidov（EKL）增强的 TDE 吸积率（$\\dot{M}_{\\rm BH,TDE}=0.5m_\\star\\dot{N}_{\\rm TDE}$）。", "assumptions": [ "每次 TDE 事件中恒星质量的 50% 被中心黑洞吸积（$\\dot{M}_{\\rm BH,TDE}=0.5m_\\star\\dot{N}_{\\rm TDE}$）", "并合双黑洞假定为非自旋，引力波反冲速度采用无自旋数值拟合公式（构成了 GW recoil 效应的理论下限）" ], "limits": [ "受限于 $12.5\\,h^{-1}{\\rm cMpc}$ 的模拟体积和局部极端过密区约束条件，难以完全统计低密度与大尺度宇宙环境中的多样性" ], "citation_leads": [ "ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological Simulations: “MBH seeding model”", "II.2.4 MBH Seeds in Star Clusters: “MBH Seeds in Star Clusters”", "II.2.6 TDEs in Star Clusters: “TDEs in Star Clusters”", "II.2.7 Gravitational Wave Recoil: “Gravitational Wave Recoil”", "IV.8 TDE Contribution to MBH Early Growth: “TDE Contribution to MBH Early Growth”", "Appendix C Validation of the Constrained Realization: “Validation of the Constrained Realization”" ], "research_progress": "展示了星团失控碰撞成种可自然拓展黑洞种子至 $10^3\\,M_\\odot$，单晕内多种子原位产生使 $z=6$ 处的 MBH 并合率提升两个数量级，且早期 TDE 光度 $L_{\\rm peak} \\sim 10^{42}-10^{43}\\,{\\rm erg\\,s^{-1}}$ 为高红移暗弱黑洞提供了关键瞬态高能探测窗口。", "figures": [ { "url": "/arxiv-figures/2610.12398/SchematicPipeline_oneline.png", "caption": "Figure 1: A schematic illustration of our star-cluster-based MBH seeding model, described in full in Section II.2.1 to II.2.4 . In our cosmological hydrodynamic simulations, we first identify StarFOF structures using a FoF algorithm with star particles as the primary linking particles. We then use the star particles younger than 100 Myr and bound to the local potential within each StarFOF to determine the total mass budget of the star clusters. We use the model developed in Kruijssen [71] and calculate a cluster formation efficiency Γ \\Gamma based on the local environment of each eligible star particle. The star cluster population is then sampled from a power-law ICMF and assigned sizes and metallicity. We use the model from Williams et al. [142] to predict the BH seed mass formed in each star cluster. Finally, we seed the MBH in the simulation by converting high- Γ \\Gamma and low-metallicity star particles into BH particles.", "label": "Fig. 1", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true }, { "url": "/arxiv-figures/2610.12398/SC_BH_CoEvolution_withspiral.png", "caption": "Figure 2: A schematic illustration of the star cluster and MBH coevolution model, which is described in full in Sections II.2.5 to II.2.7 . After a cluster forms, we trace its evolution caused by stellar evolution, two-body relaxation, and TDEs. This evolution makes the star cluster less compact and less massive. The MBH is fed by TDEs, whose rate is determined by the evolved star cluster properties, and can be boosted within binary systems. After the merger, we compare the escape velocity v esc v_{\\rm esc} of the cluster and the GW recoil velocity v recoil v_{\\rm recoil} assuming zero spin for MBHs to determine whether the cluster retains the merger remnant.", "label": "Fig. 2", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12450", "revision": 1, "title": "Discovery of Hidden Extragalactic Pulsars in the Parkes Archival Data", "abstract": "Just over 1% of the known radio pulsar population resides in the Large and Small Magellanic Clouds (MCs), the satellite galaxies that are 50-62 kpc distant from the Milky Way. These pulsars are important for constraining the peak of the pulsar luminosity function, and may give insights into neutron star populations formed from stars of different metallicities than the Milky Way. Using search techniques that have proven highly effective at discovering a large number of pulsars in archival data by folding candidates near the noise floor at high harmonic folds, we reprocessed the original Parkes Multibeam MC surveys and discovered six pulsars. Five of these pulsars are located in the Large Magellanic Cloud (LMC), including one with a spin period of 3.8s, making it the slowest pulsar known in the MCs. The remaining pulsar was detected toward the Small Magellanic Cloud (SMC), and is associated with the Milky Way foreground. Four of the newly discovered pulsars exhibit scintillation, with one showing clear nulling and others showing possible nulling behavior. These discoveries bring the total number of radio pulsars known in the LMC to 49. A luminosity function and duty cycle analysis of all current MC pulsars shows that they are consistent with Galactic canonical pulsars. Population synthesis simulations suggest that deeper surveys would reveal many more pulsars in the MCs, including up to handful of millisecond pulsars, based on the adopted upper limits for their parent populations. Finally, this reprocessing demonstrates the continued importance of reanalyzing archival data, both to improve the completeness of pulsar surveys and detect scientifically valuable objects.", "published": "2026-10-08T17:58:46Z", "updated": "2026-10-08T17:58:46Z", "authors": [ "Rahul Sengar", "Laila Vleeschower", "Matthew Bailes", "Fronefield Crawford", "Duncan R. Lorimer", "Joshua P. Ridley" ], "url": "https://arxiv.org/abs/2610.12450v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12450", "revision": 1, "status": "ready", "source_fingerprint": "881a5303d23b7f432be0998d555eb946f119382fe78da4874f6be5b9ba84ffc3", "priority": "worth_knowing", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12450v1", "inspected_sections": [ "Introduction", "Discovery of Hidden Extragalactic Pulsars in the Parkes Archival DataFacilities: Parkes/Murriyang radio telescope", "I Introduction", "II Data reduction and periodicity searches", "II.1 FFT based periodicity searches", "II.2 FFA-based periodicity searches", "III Results", "III.1 PSR J0443–68", "III.2 PSR J0506–66", "III.3 PSR J0520–67", "III.4 PSR J0541–68", "III.5 PSR J0543–67", "III.6 PSR J0051–75", "IV Discussion", "IV.1 Known pulsar redetections", "IV.2 Association of the new pulsars with the LMC", "IV.3 Flux densities and Luminosities", "IV.4 Duty Cycle–Period Relation", "IV.5 Population synthesis study of the MCs", "V Conclusions", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12450v1", "locator": "Introduction; Discovery of Hidden Extragalactic Pulsars in the Parkes Archival DataFacilities: Parkes/Murriyang radio telescope; I Introduction; II Data reduction and periodicity searches; II.1 FFT based periodicity searches; II.2 FFA-based periodicity searches; III Results; III.1 PSR J0443–68; III.2 PSR J0506–66; III.3 PSR J0520–67; III.4 PSR J0541–68; III.5 PSR J0543–67; III.6 PSR J0051–75; IV Discussion; IV.1 Known pulsar redetections; IV.2 Association of the new pulsars with the LMC; IV.3 Flux densities and Luminosities; IV.4 Duty Cycle–Period Relation; IV.5 Population synthesis study of the MCs; V Conclusions; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "dc992d28b531b87637e903fd66a5aadf49bf9b5c1b89d2fab429fa0547b81b02" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:23:42.876Z", "reason": "该工作利用改进的周期搜索流程重新挖掘 Parkes 麦哲伦云存档数据，发现了 5 颗大麦哲伦云脉冲星和 1 颗前景脉冲星，给出了河外脉冲星光度函数幂律斜率与银河系的统计一致性，为河外致密天体族群分布及星系际/银晕色散测量基线提供了重要样本支持。", "result": "在 Parkes 存档数据中新证认 6 颗脉冲星，其中 5 颗位于大麦哲伦云（LMC），包含 LMC 最慢脉冲星 PSR J0520$-$67（$P=3.8\\,\\mathrm{s}$, $\\mathrm{DM}=150\\,\\mathrm{pc\\,cm^{-3}}$）。5 颗 LMC 脉冲星在 1.4 GHz 的流量密度为 $26\\text{--}60\\,\\mu\\mathrm{Jy}$，对应伪光度 $L_{1400} \\sim 65\\text{--}150\\,\\mathrm{mJy\\,kpc^{2}}$。高光度尾端（$L_{1400} > 125\\,\\mathrm{mJy\\,kpc^{2}}$）累积光度函数 $\\log N(>L) = \\alpha \\log L + C$ 拟合表明，MC 样本斜率 $\\alpha = -1.20 \\pm 0.02$ 与银河系（$\\alpha = -1.30 \\pm 0.01$）在统计上保持一致。", "reading_entry": "IV.3 Flux densities and Luminosities", "problem": "由于河外距离带来的微弱流量密度及星系际/银道面弥散效应，麦哲伦云中大量慢脉冲星与窄占空比脉冲星在早期巡天处理中被红噪声与庞大候选体掩盖，制约了对不同金属丰度星系下脉冲星光度函数和族群合成模型的精确检验。", "method": "利用 PRESTO `rfifind` 滤除 RFI 后，通过 GPU 加速程序 PEASOUP 执行 FFT 周期搜索（$\\mathrm{DM} \\le 500\\,\\mathrm{pc\\,cm^{-3}}$，最大线性加速度 $|a| = 25\\,\\mathrm{m\\,s^{-2}}$），并结合 riptide 执行 FFA 快速折叠搜索。利用辐射计方程估算最小探测流量 $S_{\\rm min} = \\frac{(S/N)\\,\\beta\\,(T_{\\rm rec}+T_{\\rm sky})}{G\\,\\sqrt{n_{\\rm pol}\\,\\Delta\\nu\\,t_{\\rm int}}}\\,\\sqrt{\\frac{\\delta}{1-\\delta}}$，并利用 PsrPopPy 开展星族合成模拟。", "assumptions": [ "假设 LMC 脉冲星平均距离为 $50\\,\\mathrm{kpc}$，SMC 脉冲星平均距离为 $62\\,\\mathrm{kpc}$。", "假设双星脉冲星在观测积分时间内的加速度在相干搜索限 $|a| \\le 25\\,\\mathrm{m\\,s^{-2}}$ 内保持近似恒定。" ], "limits": [], "citation_leads": [ "II.1 FFT based periodicity searches: “Linear acceleration searches were carried out up to a maximum acceleration of $|a|=25~\\rm m\\,s^{-2}$, which provides coherent sensitivity to binary pulsars with orbital periods of the order of one day”", "III.3 PSR J0520–67: “PSR J0520$-$67 is notable for being the slowest spinning radio pulsar known in either the SMC or LMC with a spin period of $P=3.8$ s and a $\\mathrm{DM}=150~\\mathrm{pc\\,cm^{-3}}$.”", "IV.3 Flux densities and Luminosities: “At an assumed LMC distance of $\\sim$50 kpc, these correspond to luminosities of $L_{1400}\\sim 65$–150 mJy kpc2, and are close to the median of the known LMC pulsar population”", "IV.5 Population synthesis study of the MCs: “Sky positions were drawn from two-dimensional Gaussian distributions centered on the respective Clouds and were used to determine whether a pulsar lies within the survey footprint”" ], "research_progress": "将已知的 LMC 射电脉冲星样本提升至 49 颗，拓展了河外长周期电波脉冲星极限（$P=3.8\\,\\mathrm{s}$），并在 $\\sim 15\\%$ 相对误差水平上确认了麦哲伦云脉冲星在 1.4 GHz 下的光度函数尾端幂律指数与银河系一致。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } } ], "skip": [ { "arxiv_id": "2610.10669", "revision": 1, "title": "Impact of site-dependent noise configurations on Einstein Telescope science at low frequency", "abstract": "We investigate how site-dependent Newtonian noise configurations affect the scientific performance of the Einstein Telescope (ET), a third-generation gravitational-wave observatory. We compare the baseline triangular and 2L detector geometries, with arm lengths of 10km and 15km, respectively, under three site-dependent noise scenarios constructed from measurements in the Euregio Meuse-Rhine region, Lausitz, and Sardinia. The differences among the adopted sensitivities are concentrated mainly below 10Hz and thus have the greatest impact on science cases that rely on the early inspiral of light objects, or on massive systems whose characteristic frequencies lie in the low-frequency band. We quantify these effects for four ET science cases: (1) detection and parameter estimation of intermediate-mass black-hole binaries; (2) post-Newtonian tests of General Relativity based on the early inspiral; (3) black-hole ringdown spectroscopy with massive remnants; and (4) early-warning and sky-localization capabilities for binary neutron-star mergers. Using Bayesian parameter estimation, we find that improved low-frequency sensitivity can significantly enhance ET's scientific performance across all four cases. Within the configurations considered here, a 2L network in which at least one of the two L-shaped interferometers attains a noise level comparable to that assumed for the Sardinian site generally provides better performance than the triangular configurations. Conversely, strong degradation of the sensitivity below 10Hz can substantially reduce, and in some regimes offset, the scientific gains expected from increasing the arm length from 10km to 15km. These results highlight the importance of site selection and low-frequency noise mitigation, alongside network geometry, for fully realizing ET's scientific potential in the largely unexplored frequency band below 10Hz.", "published": "2026-10-07T18:00:00Z", "updated": "2026-10-07T18:00:00Z", "authors": [ "Francesco Crescimbeni", "Matteo Di Giovanni", "Davide Rozza", "Andrea Contu", "Alessandro Cardini", "Domenico D'Urso", "Carlo Giunchi", "Luca Naticchioni", "Marco Olivieri", "Mike Lindner", "Andreas Rietbrock", "Paolo Pani" ], "url": "https://arxiv.org/abs/2610.10669v1", "categories": [ "gr-qc", "astro-ph.CO", "astro-ph.HE", "astro-ph.IM", "nucl-th" ], "primary_category": "gr-qc", "analysis": { "arxiv_id": "2610.10669", "revision": 1, "status": "ready", "source_fingerprint": "535be40d26fac1db9f91f287416664b730da7313e3b298ffc094a243d6919310", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10669v1", "inspected_sections": [ "Introduction", "1 Introduction", "2 Detector networks", "3 Methods", "4 Results", "5 Conclusions", "6 Appendix" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10669v1", "locator": "Introduction; 1 Introduction; 2 Detector networks; 3 Methods; 4 Results; 5 Conclusions; 6 Appendix", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "aaa0f10f72781373b1ec77c1afec23375f475e0e71c4561d6252a86fac4ba5ed" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:03:14.455Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "1 Introduction", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “We investigate how site-dependent Newtonian noise configurations affect the scientific performance o”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10675", "revision": 1, "title": "Kinematic and Dynamical Properties of Solar Neighborhood White Dwarfs from SDSS DR19 and Gaia DR3", "abstract": "We present a comprehensive kinematic and dynamical analysis of 5,837 DA white dwarfs with SDSS DR19 spectroscopy and Gaia DR3 astrometry. Using complementary spatial distributions, kinematic properties, and orbital parameters, we show that the sample is overwhelmingly dominated by the thin disk, with only minor contributions from the thick disk and the halo. Velocity dispersions and orbital eccentricities increase systematically from the thin disk to the halo, reflecting progressively hotter Galactic populations. Total stellar ages available for 4,829 white dwarfs reveal a clear age-velocity dispersion relation with power-law indices of 0.06-0.17, confirming that white dwarfs preserve the secular dynamical heating history of the Galactic disk. We derive a thin-disk scale-height of 123-229 pc and radial scale-length of 3.2-3.5 kpc, while the thick disk has a scale height of 865 pc and contributes approximately 6-7 % of the local stellar density. Reconstructed birth radii indicate that changes in the guiding radii represent an important component of the present-day radial redistribution of nearby white dwarfs, although the relative contributions of radial migration and orbital blurring cannot be uniquely separated from these displacement measures. These results establish white dwarfs as powerful tracers of the kinematic, dynamical, and structural evolution of the Milky Way.", "published": "2026-10-07T18:00:00Z", "updated": "2026-10-07T18:00:00Z", "authors": [ "O. Caliskan", "M. Kilic", "S. Bilir" ], "url": "https://arxiv.org/abs/2610.10675v1", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.10675", "revision": 1, "status": "ready", "source_fingerprint": "6e9a144b69ac610a446f8424b8c4b6ae3be360f900c7569c8fd929343011a0e5", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10675v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10675v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.271Z", "reason": "论文研究太阳邻域白矮星的银河系运动学、动力学与结构演化，没有涉及指定的高能瞬变、致密天体高能观测或相关环境问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “These results establish white dwarfs as powerful tracers of the kinematic, dynamical, and structural evolution of the Milky Way.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10676", "revision": 1, "title": "Global and Local Infall in the ASHES Sample (GLASHES). III. Physical Parameters of Contracting Motion onto Dense Cores in 70 $μ$m Dark Massive Clumps", "abstract": "Core growth is a key process in high-mass star formation. As part of the GLASHES (Global and Local Infall in the ASHES Sample) survey, we present infall velocities and mass infall rates derived from blue-asymmetric line profiles toward cores embedded in massive 70 \\textmu m-dark clumps. Robust Hill5 model fits were obtained for 70 of the 135 cores exhibiting blue-asymmetric profiles, yielding infall velocities of 0.11--1.60 km s$^{-1}$ and mass infall rates ranging from $\\sim$10$^{-5}$ to $5\\times10^{-3}\\,M_\\odot\\,{\\rm yr}^{-1}$. Both quantities increase systematically from prestellar candidates to warm cores and outflow-associated cores. The inferred infall velocities are close to the cores' free-fall velocities (mean $v_{\\rm in}/v_{\\rm ff}\\sim0.75$) and $t_{\\rm in}=R/v_{\\rm in}$ is comparable to the free-fall time, indicating dynamical fast contraction. Hill5 infall velocity correlates moderately with the non-thermal velocity dispersion and Mach number measured from optically thin tracers, indicating that organized infall contributes to the observed line widths. The mass infall rate follows a power-law relation with core mass, $\\dot{M}=1.3\\times10^{-4}\\,(M/M_\\odot)^{0.83\\pm 0.06}\\,M_\\odot\\,{\\rm yr}^{-1}$, across $0.1\\,M_\\odot \\lesssim M \\lesssim 30\\,M_\\odot$. The power-law index increases from $\\sim$0.65 for prestellar cores to $\\sim$1.10 for outflow-associated cores, likely tracing an evolution in the dominant physical process. The Hill5 infall velocities and mass infall rates for the GLASHES cores are larger than those of cores in nearby low-mass star forming regions but smaller than those of larger scale high-mass clumps. These results provide the first statistical constraints on core-scale mass accumulation during the earliest stages of high-mass star formation.", "published": "2026-10-07T18:00:00Z", "updated": "2026-10-07T18:00:00Z", "authors": [ "Kaho Morii", "Patricio Sanhueza", "Qizhou Zhang", "Philip C. Myers", "James M. Jackson", "Fumiaki Yoshida" ], "url": "https://arxiv.org/abs/2610.10676v1", "categories": [ "astro-ph.GA", "astro-ph.SR" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10676", "revision": 1, "status": "ready", "source_fingerprint": "08e35bdcba73740ac134ac88d3f2b873d3420496ef8fc374445ac7e196a55231", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10676v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10676v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.272Z", "reason": "论文关注高质量恒星形成区致密核的吸积与收缩，不涉及指定的高能瞬变天体物理方向；其质量吸积标度与超新星中心引擎或致密天体环境无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The mass infall rate follows a power-law relation with core mass, $\\dot{M}=1.3\\times10^{-4}\\,(M/M_\\odot)^{0.83\\pm 0.06}\\,M_\\odot\\,{\\rm yr}^{-1}$”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10680", "revision": 1, "title": "Exemplary Merging Clusters II: XMM-Newton and Chandra X-ray Observations of MACS J1752.0+4440 and ZwCl 1856.8+6616", "abstract": "Using deep XMM-Newton and Chandra observations, we compare the double-radio-relic galaxy cluster mergers MACS J1752.0+4440 and ZwCl 1856.8+6616. Both are 1:1 mass-ratio mergers with similar relic separations but differing nearly an order of magnitude in total mass. In MACS J1752.0+4440, the surface-brightness discontinuity at the northeastern relic yields Mach $M_ρ=1.4\\pm0.2$, while the temperature jump provides a weaker constraint, corresponding to $M_{kT}\\lesssim2.3$ at the $2σ$ level, lower than the radio-derived $M_{\\rm radio}=3.1\\pm0.1$. No discontinuity is detected at the southwestern relic. Thermodynamic maps and axial profiles reveal surviving relatively low-entropy cores embedded in Mpc-scale stripped-gas structures. The nearly uniform X-ray tail brightness and a southwestern plateau coincident with a third lensing mass peak favor a non-zero impact parameter and complex assembly history. In ZwCl 1856.8+6616, we do not detect a clear surface brightness discontinuity at either relic. The northern X-ray peak leads its brightest cluster galaxy (BCG) and lensing peak, while the hotter southern X-ray peak is laterally offset from its BCG and lensing peak. The asymmetric intracluster emission favors a phase near or after first apocenter, when displaced gas can develop a slingshot-like morphology. We present two TNG-Cluster analogs in which a minor merger followed by an off-axis major collision produces extended X-ray tails resembling MACS J1752.0+4440 and later leads to gas structures resembling ZwCl 1856.8+6616. X-ray morphology independently confirms the merger phases inferred from relic-based chronometry, placing MACS J1752.0+4440 before and ZwCl 1856.8+6616 after first apocenter, and demonstrating that similar relic and lensing configurations can correspond to distinct dynamical states.", "published": "2026-10-07T18:00:01Z", "updated": "2026-10-07T18:00:01Z", "authors": [ "K. HyeongHan", "K. Finner", "W. Lee", "E. Silich", "W. Forman", "C. Jones", "A. Tümer", "S. Randall", "J. ZuHone", "M. James Jee", "D. Wittman", "R. J. van Weeren", "M. Troxel" ], "url": "https://arxiv.org/abs/2610.10680v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10680", "revision": 1, "status": "ready", "source_fingerprint": "ae4ebed1cbec55051bc8ff15b316519043bb7d52819a1343d83d0413c76e2391", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10680v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10680v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.273Z", "reason": "论文研究星系团并合及其射电遗迹对应的星系团尺度激波和 X 射线形态，与所列超新星或致密天体相关的激波、喷流及高能瞬变研究没有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Using deep XMM-Newton and Chandra observations, we compare the double-radio-relic galaxy cluster mer”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10683", "revision": 1, "title": "A Multi-dimensional Analysis of the Open Clusters NGC 2423 and NGC 2482 with Gaia DR3", "abstract": "We present a homogeneous photometric, astrometric, and kinematic study of the Hyades-like open clusters NGC 2423 and NGC 2482 based on Gaia DR3 data. Cluster memberships are determined using the UPMASK algorithm in the multi-dimensional parameter space of (alpha, delta, parallax, mu_alpha cos(delta), mu_delta), with radial velocities incorporated when available. Gaussian modelling of the astrometric distributions yields mean trigonometric parallaxes of 1.060 +/- 0.035 mas and 0.735 +/- 0.061 mas, corresponding to astrometric distances of 944 +/- 31 pc and 1361 +/- 113 pc for NGC 2423 and NGC 2482, respectively. Fundamental parameters are derived through PARSEC isochrone fitting, resulting in ages of 1250 +/- 100 Myr and 445 +/- 50 Myr, observed distance moduli (m-M)_obs = 9.90 +/- 0.10 and 10.80 +/- 0.20 mag, and reddening values E(G_BP-G_RP) = 0.07 +/- 0.01 and 0.10 +/- 0.02 mag, equivalent to E(B-V) = 0.054 and 0.078. The corresponding photometric distances are 892 +/- 50 pc and 1311 +/- 146 pc. We further investigate the internal and global kinematics of both clusters using velocity-ellipsoid parameters, the convergent-point method, and action-angular-momentum diagnostics. The derived kinematic properties show that NGC 2482 closely matches the velocity-space characteristics of the Hyades stream, while NGC 2423 shares the characteristic rotational velocity and angular momentum of the Hyades-like population but is offset in its U component. Both clusters occupy the angular-momentum range associated in the literature with Hyades-like clusters and bar-related resonances, although this association is based on their present-day kinematics and action-space locations rather than a direct dynamical demonstration of resonance trapping.", "published": "2026-10-07T18:00:02Z", "updated": "2026-10-07T18:00:02Z", "authors": [ "W. H. Elsanhoury", "Deniz Cennet Çınar", "A. Ahmed" ], "url": "https://arxiv.org/abs/2610.10683v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10683", "revision": 1, "status": "ready", "source_fingerprint": "a3acf48ada8d700dc97bce0b2b707acd3f58efe95abc1901007831c42577cf14", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10683v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10683v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.273Z", "reason": "论文聚焦疏散星团的 Gaia 天体测量、光度和运动学性质，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We present a homogeneous photometric, astrometric, and kinematic study of the Hyades-like open clusters NGC 2423 and NGC 2482”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10687", "revision": 1, "title": "Cosmic Duets II. Growth and accretion in Gaia Multi-Peak dual AGN at Cosmic Noon", "abstract": "We present the first statistical characterization of the physical properties of Cosmic Duets: dual AGN in the redshift range 0.5 $\\leq$ z $\\leq$ 3.0 with projected separations of 1-7 kpc, corresponding to systems in which both AGN are expected to reside within the same merger remnant. We analyze the largest homogeneous sample currently available, consisting of 30 spectroscopically confirmed Cosmic Duets selected via the Gaia Multi-Peak technique. Using rest-frame UV-to-optical integral-field spectroscopy for all targets, primarily with VLT/MUSE, VLT/ERIS, and Keck/OSIRIS, we spatially resolve the two AGN components and extract separate spectra for each system. We decompose the continuum, emission lines, and Fe II complexes through spectral fitting. We derive black hole masses of log($M_{BH}/M_{sun}$) ~ 7.4-10.1 and bolometric luminosities of log($L_{bol}/erg s^{-1}$) ~ 44.8-47.2, consistent with those of single AGN at similar redshifts. We finally carry out the first comparison of dual AGN properties with semi-analytical models and hydrodynamical simulations, including L-GalaxiesBH and Astrid. Astrid provides a closer match to the observed black-hole mass-ratio distribution, but its selected systems are predominantly at lower redshifts, resulting in lower bolometric luminosities at fixed G-band magnitude. L-GalaxiesBH perfectly reproduce the observed parameter space, but it predicts more heterogeneous pairs, with higher primary-bolometric luminosity, lower-mass secondary SMBHs, and higher Eddington ratios, resulting in an excess of near-Eddington accreting AGN due to its adopted accretion prescription. Our results suggest that, in GMP-selected systems, secondary SMBH growth is more efficient than predicted by current models, leading to more comparable black-hole masses and accretion power between the two components.", "published": "2026-10-07T18:00:02Z", "updated": "2026-10-07T18:00:02Z", "authors": [ "M. Scialpi", "F. Mannucci", "D. Izquierdo-Villalba", "A. Marconi", "J. Singh", "M. Volonteri", "C. Marconcini", "Q. D'Amato", "B. Moreschini", "M. V. Zanchettin", "G. Tozzi", "M. Ceci", "L. Ulivi", "E. Bertola", "S. Bonoli", "C. Bracci", "E. Cataldi", "C. Cicone", "A. Ciurlo", "M. Colpi", "G. Cresci", "A. De Rosa", "M. Dotti", "M. Fumagalli", "M. Ginolfi", "I. Lamperti", "E. Nardini", "M. Parvatikar", "M. Perna", "F. Rigamonti", "K. Rubinur", "B. Sala", "A. Sesana", "P. Severgnini", "C. Spingola", "D. Spinoso", "G. Venturi", "C. Vignali", "S. Yeh" ], "url": "https://arxiv.org/abs/2610.10687v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10687", "revision": 1, "status": "ready", "source_fingerprint": "ccd9009fc32f2cdd2c2909461921b163bdce6363b27f105d6430da895d93bbbe", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10687v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10687v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.273Z", "reason": "论文研究宇宙正午时期双 AGN 的黑洞增长、吸积及其与星系形成模型的比较；虽涉及 AGN，但摘要未显示与指定的瞬变、相对论喷流或致密天体高能观测方向有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We present the first statistical characterization of the physical properties of Cosmic Duets: dual AGN in the redshift range 0.5 $\\leq$ z $\\leq$ 3.0”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10689", "revision": 1, "title": "Discovery of a Nearby Ultra-fast Magnetic White Dwarf Propeller: Common Pathways to Magnetic Cataclysmic Variables", "abstract": "The fastest spinning white dwarfs (WDs), which approach break-up speeds, are found in close binary systems. In the two known magnetic WD ``propellers'', AE~Aqr and LAMOST J0240+1952, the magnetic WD spins so rapidly that it ejects the material transferred by its Roche-lobe-filling companion rather than accreting it. We report the discovery of the third such system, 1eRASS J042633.5$-$250226 (1eRASS J0426/Valeria), at only 265 pc, identified by combining SRG/eROSITA and \\textit{Gaia} data via the ``X-ray Main Sequence''. TESS photometry shows AE~Aqr-like flaring and orbital modulation with $P_{\\mathrm{orb}} \\approx 6.62$ hr, and ZTF shows month-long high/low state changes. Phase-resolved Palomar/DBSP spectroscopy confirms the orbital period and yields a donor radial velocity of $K_2 = 202\\pm7$ km s$^{-1}$. High-speed Palomar/CHIMERA photometry detects optical pulsations on three nights with the strongest detection at $P_\\textrm{spin} = 26.8$ sec, though further observations are needed to confirm this as the WD spin. Spectral fitting of the donor in the low state reveals a late K-type star with $T_{\\mathrm{donor}} = 4100\\pm150$ K. Zeeman splitting in the optical spectrum yields a candidate field strength of $B_{\\mathrm{WD}} = 26 \\pm 3$ MG, meaning the system will evolve into a polar. Like other WD propellers, the system is X-ray faint ($L_X \\approx 7\\times 10^{30}$ erg s$^{-1}$), but is not detected in the radio, and a spin period is not detected in X-rays by SRG/eROSITA. The proximity of this system and evolutionary model constraints on the timeframe of the propeller phase yield a birth rate density of $\\sim8\\times10^{-16} \\textrm{pc}^{-3} \\textrm{yr}^{-1}$, which agrees with that of magnetic CVs, suggesting that a substantial fraction of magnetic CVs pass through a propeller phase.", "published": "2026-10-07T18:00:02Z", "updated": "2026-10-07T18:00:02Z", "authors": [ "Antonio C. Rodriguez", "Kareem El-Badry", "R. Michael Rich", "Kevin N. Ortiz Ceballos", "Ingrid Pelisoli", "Casey J. Law", "Kaya Mori", "Boris Gaensicke", "Edo Berger", "Liam Connor", "Ilkham Galiullin", "Ilaria Caiazzo", "Matthew Graham", "Samuel Whitebook" ], "url": "https://arxiv.org/abs/2610.10689v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10689", "revision": 1, "status": "ready", "source_fingerprint": "e6d9395c775b6b0583547a58d5237774251800a78c4e7afbd6fc50215713adda", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10689v1", "inspected_sections": [ "Introduction", "Discovery", "Archival Photometry", "Multiwavelength Follow-up", "Optical High-Speed Photometry", "Optical Spectroscopy", "X-ray", "Radio Campaign", "Binary Parameters", "Radial-Velocity Analysis", "Spectral Energy Distribution", "Lower limit on the WD mass from the spin period", "No accretion disk: trailed H$alpha$ and Doppler tomogram", "Joint binary parameters", "Magnetic field from Zeeman splitting", "Confirmation of propeller mode", "Discussion", "The propeller population: stripped, out-of-equilibrium donors", "Space density and birth rate", "State changes", "Conclusion", "Acknowledgments", "TESS orbital modulation", "X-ray spectral analysis", "Donor temperature from the low-state spectrum", "Alternative Zeeman field solution at 33 MG", "CHIMERA pulsation searches on additional nights", "Lick/Shane spectroscopy", "MCMC corner plots" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10689v1", "locator": "Introduction; Discovery; Archival Photometry; Multiwavelength Follow-up; Optical High-Speed Photometry; Optical Spectroscopy; X-ray; Radio Campaign; Binary Parameters; Radial-Velocity Analysis; Spectral Energy Distribution; Lower limit on the WD mass from the spin period; No accretion disk: trailed H$alpha$ and Doppler tomogram; Joint binary parameters; Magnetic field from Zeeman splitting; Confirmation of propeller mode; Discussion; The propeller population: stripped, out-of-equilibrium donors; Space density and birth rate; State changes; Conclusion; Acknowledgments; TESS orbital modulation; X-ray spectral analysis; Donor temperature from the low-state spectrum; Alternative Zeeman field solution at 33 MG; CHIMERA pulsation searches on additional nights; Lick/Shane spectroscopy; MCMC corner plots", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "4ec84eff64ed079a4ba2f58d7dd07357653c9ea462ba6842bfeb7f49a6cf9170" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:05:05.642Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "先检查摘要，再按需打开原文。", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “The fastest spinning white dwarfs (WDs), which approach break-up speeds, are found in close binary s”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [ { "url": "/arxiv-figures/2610.10689/tess.png", "caption": "Figure 3: TESS light curve of 1eRASS J0426/Valeria ( black ) folded on the 6.616-hr orbital period, showing ellipsoidal orbital variability superposed with high-amplitude flares similar in morphology to AE Aqr (9.88-hr orbital period).", "label": "Fig. 3", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false }, { "url": "/arxiv-figures/2610.10689/ztf.png", "caption": "Figure 4: Long-baseline ZTF g g - and r r -band photometry of Valeria ( bottom panel ), with the epochs of all follow-up and archival observations marked ( top panel ): optical spectroscopy (Palomar/DBSP, open diamonds, 2024 Aug 30 and Nov 9; Lick/Kast, open circles, 2024 Oct 7, 2024 Nov 28, 2025 Dec 16) and high-speed photometry (Palomar/CHIMERA, filled triangles; 2024 Sep 3, Sep 30, Oct 24); X-ray (SRG/eROSITA eRASS1 scan, star; 2020 Feb 28); and radio (ASKAP archival epochs, open circles; MeerKAT archival epoch, open square; VLA, filled cross; 2026 Jan 6). Dotted vertical lines extend each epoch down through the light curve. The TESS Sector 31 window (2020 Oct 22 – Nov 16) is shaded grey. The system transitions between an active (flaring) high state and a quiescent low state on ∼ \\sim few month- to year-long timescales.", "label": "Fig. 4", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10691", "revision": 1, "title": "Accreting Neutron Stars in Low-Mass X-ray Binaries", "abstract": "Neutron star low-mass X-ray binaries (NS LMXBs) are systems in which a neutron star accretes matter from a Roche-lobe-filling companion via an accretion disc, releasing gravitational energy with an efficiency of order 10-20% of the rest-mass energy. Unlike black holes, neutron stars possess a solid surface and a magnetic field, making NS LMXBs uniquely rich laboratories for high-energy astrophysics and dense-matter physics. In this chapter we review the current understanding of accretion onto neutron stars in LMXBs, tracing matter from the outer disc radii to the stellar surface across five decades of observational discovery. We survey the principal classes of accreting neutron star systems - canonical atoll and Z-sources, ultracompact X-ray binaries, accreting millisecond pulsars, and transitional millisecond pulsars - and discuss how their spectral states, timing properties, and multiwavelength behaviour encode the physics of the inner accretion flow. We examine thermonuclear Type-I X-ray bursts as probes of nuclear burning and neutron star structure, and review the boundary and spreading layers where accreted matter decelerates onto the stellar surface. We discuss relativistic jets and ionised disc winds as regulators of the accretion-ejection cycle. Finally, we present X-ray polarimetric results from the Imaging X-ray Polarimetry Explorer (IXPE), which for the first time provide new, though model-dependent, constraints on the geometry of the emission regions - disc, corona, spreading layer, and jets - that spectroscopy alone cannot resolve, alongside complementary optical and infrared polarimetric observations.", "published": "2026-10-07T18:00:03Z", "updated": "2026-10-07T18:00:03Z", "authors": [ "M. C. Baglio", "S. E. Motta", "A. P. Nitindala", "J. Poutanen" ], "url": "https://arxiv.org/abs/2610.10691v1", "categories": [ "astro-ph.HE", "astro-ph.SR" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10691", "revision": 1, "status": "ready", "source_fingerprint": "36cd64ab8d74867ea89df490257e17a93a46d741e197f4c4f2d8315f45365f5f", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10691v1", "inspected_sections": [ "Introduction", "The different flavours of accreting NSs", "Canonical NS LMXBs", "Ultracompact X-Ray binaries", "Evolutionary Pathways", "UCXBs in Globular Clusters", "Observational Signatures and Accretion Diagnostics", "Accreting Millisecond Pulsars", "Transitional millisecond pulsars", "Variability of NS XRBs", "Short timescale variability", "Type-I bursts", "Boundary layer and spreading layer in NS LMXBs", "Accretion-ejection coupling in NS LMXBs", "Jets in NS LMXBs", "Winds in NS LMXBs", "Polarization of NS LMXBs", "X-ray polarization and models", "Optical and infrared polarization", "Summary", "Declarations", "Conflict of interest" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10691v1", "locator": "Introduction; The different flavours of accreting NSs; Canonical NS LMXBs; Ultracompact X-Ray binaries; Evolutionary Pathways; UCXBs in Globular Clusters; Observational Signatures and Accretion Diagnostics; Accreting Millisecond Pulsars; Transitional millisecond pulsars; Variability of NS XRBs; Short timescale variability; Type-I bursts; Boundary layer and spreading layer in NS LMXBs; Accretion-ejection coupling in NS LMXBs; Jets in NS LMXBs; Winds in NS LMXBs; Polarization of NS LMXBs; X-ray polarization and models; Optical and infrared polarization; Summary; Declarations; Conflict of interest", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "cdb798ffc8a70588aa929c3ccfb907bc06082fe017332c3f5cd5bd415170426d" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:06:58.746Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "先检查摘要，再按需打开原文。", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “Neutron star low-mass X-ray binaries (NS LMXBs) are systems in which a neutron star accretes matter”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [ { "url": "/arxiv-figures/2610.10691/SED_pol_pulsed_orange_blue.png", "caption": "Figure 10: Spectral energy distribution of the optical/X-rays/ total (diamonds), pulsed (circles) and polarised (squares) emission of PSR J1023+0038 in the high mode of the sub-luminous disc state. Adapted from Baglio et al. (2025b) .", "label": "Fig. 10", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false }, { "url": "/arxiv-figures/2610.10691/SCO_vs_Rout1807_side_by_side_upper_limits.png", "caption": "Figure 9: Left : optical and near-infrared polarization of Sco X-1. The optical points (UBVRI bands) are taken from Schultz et al. (2004) . The dashed line is the interstellar polarization model fit to the optical; adapted from Shahbaz et al. (2008) . Right : optical PA vs. PA of MAXI J1807+132 for the three epochs. A clear rotation of the PA by approximately ∼ 100 ∘ \\sim 100^{\\circ} is observed in the R and I bands between the first two epochs and the third. Upper limits on the polarization level are reported at the 99.97 % 99.97\\% credible interval, while all other uncertainties are quoted at the ± 1 ​ σ \\pm 1\\sigma credible level. Adapted from Rout et al. (2025) .", "label": "Fig. 9", "category": "fitting", "category_badge": "数据拟合与模型对比", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10695", "revision": 1, "title": "The Origin of the Fermi Halo-like Emission: A New Model of the Fermi Bubbles", "abstract": "We study the gamma-ray sky at high latitudes for energies between 0.3 and 900 GeV. We search for a contribution in the high-latitude sky and in the region of the Galactic Stellar Halo that would be beyond known astrophysical emissions, i.e., the galactic diffuse emission, the isotropic mostly extragalactic gamma-ray background, the Fermi Bubbles, Loop I, the contribution from the Galactic Center Excess, and the known point and extended gamma-ray sources detected by the Fermi-LAT Collaboration. We perform a sequence of template fits to the Fermi gamma-ray data, testing different regions of interest of the galactic sky, utilizing a large set of alternative galactic diffuse emission models, and implementing alternative fitting schemes to assess the impact of increased modeling complexity of the gamma-ray sky. We find that the halo-like emission recently reported by Totani (2025) is real, but it is likely due to emission from the Fermi Bubbles rather than dark matter annihilation in the Galactic halo. We provide new templates for the Fermi Bubbles, including an updated model for the Flat Bubbles and a detailed model of their substructures, the Cocoons and the Inner Bubbles. In combination, these components account for the previously reported halo-like emission. We also estimate the associated fluxes and spectral properties of the Flat Bubbles, the Inner Bubbles, and the Cocoons. This updated model for the Fermi Bubbles provides new input toward understanding their origin.", "published": "2026-10-07T18:00:05Z", "updated": "2026-10-07T18:00:05Z", "authors": [ "Ilias Cholis", "Leo Qiyuan Hu", "Yi-Ming Zhong" ], "url": "https://arxiv.org/abs/2610.10695v1", "categories": [ "astro-ph.HE", "astro-ph.CO", "hep-ph" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10695", "revision": 1, "status": "ready", "source_fingerprint": "0c75606957c694e3c48bd30e96bc58d78f240fbb6ceb031958f42ae892187fcc", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10695v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10695v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.274Z", "reason": "论文研究高纬伽马射线天空中的类晕发射及费米气泡模板，主要涉及银河系伽马射线背景建模；摘要未显示其与指定的瞬变天体、中心引擎或致密天体观测方向有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We find that the halo-like emission recently reported by Totani (2025) is real, but it is likely due to emission from the Fermi Bubbles rather than dark matter annihilation in the Galactic halo.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10698", "revision": 1, "title": "A \"universal\" supernova efficiency to drive the HI turbulence in nearby star-forming galaxies", "abstract": "The origin of cold gas turbulence in galaxies has long been debated. Supernovae (SNe), the dominant form of stellar feedback, were thought insufficient to sustain it against dissipation, especially in galactic environments with low star formation rates (SFRs). We investigate the origin of the neutral atomic gas (HI) turbulence in dwarf irregular galaxies, a challenging regime of low masses and SFRs. We build on a recent study of spirals showing that disc flaring prolongs the dissipation timescale, reducing the energy needed to sustain turbulence and making SN feedback viable. We measure the SN efficiency, that is the fraction of SN energy required to sustain HI turbulence, in 14 dwarfs, and test whether a \"universal\" efficiency holds across a sample representative of the star-forming main sequence. From the observed HI distributions and kinematics, we derive the radial profiles of the HI kinetic energy per unit area and model them as the sum of thermal energy and turbulent energy from SNe, constrained by the observed SFR surface density. We consider pure cold and warm neutral medium (WNM) phases as limiting cases, as well as a mixed two-phase scenario, obtaining the SN efficiency and WNM fraction via hierarchical Bayesian inference. We find that the observed HI kinetic energy in dwarfs requires only $\\lesssim 3\\%$ of the SN energy, and that a \"universal\" efficiency of $\\approx 2\\%$ explains the HI turbulence across our main-sequence sample. Our findings suggest that the SN efficiency remains similar across galaxies with different properties, offering valuable constraint for feedback recipes in galaxy evolution models.", "published": "2026-10-07T18:00:06Z", "updated": "2026-10-07T18:00:06Z", "authors": [ "Lauri Sassali", "Cecilia Bacchini", "Aku Venhola", "Giuliano Iorio", "Antonino Marasco" ], "url": "https://arxiv.org/abs/2610.10698v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10698", "revision": 1, "status": "ready", "source_fingerprint": "d1384db6909b761220459d666bdd9ac336cb058501cdf2e92e651cf870f7eb5e", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10698v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10698v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.274Z", "reason": "论文讨论矮不规则星系中超新星反馈维持中性氢湍流的效率，属于星系尺度气体动力学与反馈研究；与超新星中心引擎、激波破越或周星介质相互作用等指定方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We measure the SN efficiency, that is the fraction of SN energy required to sustain HI turbulence, in 14 dwarfs”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10699", "revision": 1, "title": "Atypical White Dwarfs in Open Clusters", "abstract": "Open clusters are powerful laboratories for investigating the formation and evolution of white dwarfs (WDs), as their well-constrained ages link WDs to their progenitor stars. This is particularly valuable for atypical WDs, including magnetic WDs and those with non-hydrogen-dominated spectra, whose origins can be difficult to disentangle in the field. We assemble the largest sample to date of atypical WDs in open clusters: eight non-magnetic WDs with helium-dominated spectra, five with featureless spectra, and five magnetic WDs showing hydrogen or helium lines. We find no significant difference between the initial--final mass relations of hydrogen- and helium-atmosphere WDs, nor robust spatial or kinematic differences. The strongest difference from the field is a deficit of non-DAs between $0.8$ and $1.0\\,\\mathrm{M}_\\odot$, where the field predicts $6.0^{+0.8}_{-0.7}$ WDs, yet none are observed, with a probability of only $0.37\\%$. Massive magnetic WDs show a similar deficit: only one of 20 cluster WDs with $M_{\\mathrm{WD}}\\geq1.0\\,\\mathrm{M}_\\odot$ and $T_{\\mathrm{eff}}\\geq20{,}000\\,{\\rm K}$ is magnetic, compared with 10 of 16 in the field. Together, these deficits are consistent with an additional field population of massive merger remnants, particularly high-mass magnetic WDs and warm/hot DQs. Such objects may be underrepresented in clusters because young systems provide limited time for certain classes of delayed mergers, while older clusters lose members or dissolve; the field accumulates binary evolution products over Galactic timescales. Magnetic cluster WDs consistent with single-star evolution further suggest mass-dependent magnetic-field emergence, with fields appearing early in some massive WDs while young lower-mass WDs remain consistent with delayed emergence.", "published": "2026-10-07T18:00:06Z", "updated": "2026-10-07T18:00:06Z", "authors": [ "David R. Miller", "Ilaria Caiazzo", "Jeremy Heyl", "Pier-Emmanuel Tremblay" ], "url": "https://arxiv.org/abs/2610.10699v1", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.10699", "revision": 1, "status": "ready", "source_fingerprint": "083be7f6b58df30aca23daa1e3414590019279aa09ceba6093faac120ce402c2", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10699v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10699v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.275Z", "reason": "论文聚焦疏散星团中的白矮星人口、形成与磁场演化，与指定的高能瞬变天体及其环境研究方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We assemble the largest sample to date of atypical WDs in open clusters”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10701", "revision": 1, "title": "EK Cha b: multi-tracer detection of a protoplanet candidate in a gas-rich environment", "abstract": "Despite sustained community efforts and advances in instrumentation and high-contrast imaging, the search for protoplanets remains difficult, with only two widely accepted systems to date in Class II systems (PDS 70 and WISPIT 2). Here we present the detection of EK Cha b, a new protoplanet candidate, identified through CO emission, millimeter continuum and 0.82 micron broadband photometry, linked to EK Cha, a young late-type M star. The detection of a new protoplanet candidate offers an additional opportunity to advance our understanding of planet formation. By exploiting the wealth of archival data available for nearby star-forming regions, we aim to place EK Cha b in context, characterize its properties, and motivate future campaigns targeting similar systems. We analyzed high-spatial-resolution archival observations of EK Cha from HST, VLT/NACO, VLT/MUSE, and ALMA. We searched for EK Cha b in broadband continuum and gas tracers, reporting the measured flux with uncertainties, and upper limits for non-detections. EK Cha b shows a spectrally-resolved footprint that matches the CO J=2--1 emission, together with 0.82 micron and millimeter continuum emission. EK Cha b is spectrally resolved in CO J=2--1 emission, kinematically consistent with a circumplanetary disk. Best fits from evolutionary models place EK Cha b as a planetary mass companion, although deeper observations are required to fully confirm its nature. Although giant planets are uncommon around M dwarfs, these stars host the highest planet occurrence rate while remaining severely underrepresented in protoplanet searches. EK Cha b demonstrates that such systems are now within reach, and the advent of extremely large telescopes and improved high-contrast imaging -- where the lower host luminosity relaxes the required contras-- will open this overlooked regime to systematic exploration.", "published": "2026-10-07T18:00:06Z", "updated": "2026-10-07T18:00:06Z", "authors": [ "Felipe Alarcón", "C. Swastik", "Stefano Facchini", "Edwin A. Bergin", "Gabriele Cugno" ], "url": "https://arxiv.org/abs/2610.10701v1", "categories": [ "astro-ph.EP", "astro-ph.SR" ], "primary_category": "astro-ph.EP", "analysis": { "arxiv_id": "2610.10701", "revision": 1, "status": "ready", "source_fingerprint": "6fc89df765aa1668941a2dbdc75ec0871def5948ab4af572dcfa5b1d5ff46a74", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10701v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10701v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.275Z", "reason": "论文研究原行星候选体及其气体环境，属于行星形成研究，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Here we present the detection of EK Cha b, a new protoplanet candidate”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10719", "revision": 1, "title": "Prevalence of radio Active Galactic Nuclei in galaxy groups since z=3.5 in the COSMOS-Web field", "abstract": "Radio active galactic nuclei (AGN) are key tracers of kinetic feedback from supermassive black holes. Although the dependence of their triggering on host stellar mass is well known, the impact of the large-scale environment across cosmic time is poorly understood. We investigate the role of the environment in triggering radio AGN activity, while also studying the dependence on stellar mass ($10\\leq\\log M_{\\ast}\\,{\\rm [M_{\\odot}]}\\leq11.4$), radio luminosity ($22\\leq\\log L_{1.4}\\,{\\rm [W\\,Hz^{-1}]}\\leq26$), and redshift ($0.1\\leq z \\leq 3.5$). We combine the VLA-COSMOS 3 GHz Large Project with the COSMOS-Web galaxy and group catalogs, selecting radio-excess AGN and building radio luminosity functions (RLF) and radio AGN fractions separately for sources in galaxy groups (124 radio AGN) and in the field (405 radio AGN), out of the total of 20203 galaxies and 1678 galaxy groups. We fit the RLF to derive the cosmic evolution of radio AGN in different environments, and we provide a new parametric description of the radio AGN fractions as a function of environment, $M_{\\ast}$, $L_{1.4}$, and z. Besides confirming the known positive correlation of radio AGN fraction with host $M_{\\ast}$ in both groups and in the field, more importantly we find that the activation of a radio AGN in groups is enhanced relative to the field by a factor of 3--30 in space density and of 2 in radio AGN fraction at fixed stellar mass; the enhancement is also a function of $M_{\\ast}$, $L_{1.4}$, and z. Furthermore, in all z bins, the radio AGN fractions peak within $r \\leq 0.2R_{200}$. Overall, dense environments enhance radio AGN triggering out to at least z=3.5. We suggest the existence of a possible transition in the dominant triggering mechanism of radio AGN activity around z~1.5, potentially related to the intragroup medium in the core of groups at lower z and to merger and structure growth at earlier cosmic times.", "published": "2026-10-07T18:03:00Z", "updated": "2026-10-07T18:03:00Z", "authors": [ "F. Ubertosi", "I. Delvecchio", "I. Prandoni", "G. Toni", "G. Zamorani", "E. Daddi", "M. Gitti", "M. Sargent", "A. Traina", "C. Spingola", "F. Vito", "L. Moscardini", "G. Gozaliasl", "D. Kakkad", "W. Wang", "S. Sanjaripour", "Z. Ghaffari", "M. N. Isla Llave", "R. M. Samir", "G. Peluso", "M. Maturi", "V. Smolcic", "C. Casey", "J. Kartaltepe", "H. J. McCracken", "J. Rhodes", "B. Robertson", "M. Franco", "D. Liu", "M. Shuntov", "H. Akins", "O. Ilbert", "A. A. Khostovan" ], "url": "https://arxiv.org/abs/2610.10719v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10719", "revision": 1, "status": "ready", "source_fingerprint": "7cb567c82cd923f4c1879f877e042bdf2b1ed0b98a3179781ee799a3ccbeacd0", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10719v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10719v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.275Z", "reason": "论文考察星系群环境中射电活动星系核的发生率及其宇宙演化；摘要未涉及相对论喷流或高能瞬变观测，与目标方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We investigate the role of the environment in triggering radio AGN activity”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10721", "revision": 1, "title": "NGC 4936: abundant multi-phase medium in the central weak X-ray cool core and optically dark H I clouds in the group", "abstract": "We present a multiwavelength analysis of NGC 4936, the central galaxy of a weak cool-core group hosting an unusually large cold/warm gas reservoir. NGC 4936 contains $\\sim2\\times10^8$ M$_\\odot$ of molecular gas in a rotating disk of radius $\\sim1$ kpc, but no detected H I, with a $3σ$ upper limit of $1.13\\times10^7$ M$_\\odot$ within $\\sim2.5$ kpc. The resulting $H_2$/H I mass ratio $>17$ is consistent with a predominantly molecular medium in the high-pressure environments of central galaxies. SOAR imaging and MUSE spectroscopy reveal ionised gas extending to $\\sim15$ kpc in a complex filamentary morphology that broadly follows the molecular gas kinematics while extending well beyond the CO disk. Dust filaments similarly extend to $\\sim14$ kpc and appear to interact with a companion galaxy located only $\\sim2.5$ kpc away in projection. NGC 4936 has a star formation rate of $0.29$ M$_\\odot$ yr$^{-1}$, and its AGN shows sub-mm and X-ray variability. We favour atmospheric condensation as the primary origin of the molecular gas, although externally acquired gas may contribute. Our recalculated thermodynamic profiles reach $t_{\\rm cool}/t_{\\rm ff}\\sim25$ in the innermost region, placing the system near the threshold for multiphase condensation. The ongoing interaction may perturb the atmosphere and promote condensation while shaping the morphology and kinematics of the multiphase medium, rather than directly supplying most of the central cold gas. We additionally detect 20 H I structures in the surrounding group environment, with masses of $\\sim10^7$--$10^8$ M$_\\odot$, including several with no obvious optical counterparts.", "published": "2026-10-07T18:04:09Z", "updated": "2026-10-07T18:04:09Z", "authors": [ "Prathamesh Tamhane", "Ming Sun", "Hao Chen", "Thomas Connor", "Megan Donahue", "Mark Voit", "Mpati Ramatsoku", "Kokoro Hosogi", "Tim Edge" ], "url": "https://arxiv.org/abs/2610.10721v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10721", "revision": 1, "status": "ready", "source_fingerprint": "df133723ad54a634687b29f8de7f68332e1757306f4132caea766a32ebe4bc45", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10721v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10721v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.276Z", "reason": "论文研究星系群中心星系的多相气体、冷却与凝结；虽提及 AGN 的亚毫米和 X 射线变异，但摘要没有显示其针对高能瞬变或相关核心问题开展研究。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “its AGN shows sub-mm and X-ray variability”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10726", "revision": 1, "title": "First uGMRT Constraints on Rotation Measure in the Radio-Quiet Seyfert Galaxy NGC 4235", "abstract": "We present a multi-frequency polarimetric study of the radio-quiet Seyfert galaxy NGC 4235 using the upgraded Giant Metrewave Radio Telescope (uGMRT), aimed at constraining the Faraday rotation properties of its kpc-scale radio emission. This marks the first-ever analysis of polarization across two frequency bands of the uGMRT and the first constraints on rotation measure (RM) at lower frequencies for a weak radio source (17.1$\\pm$1.7 mJy at 1.3 GHz, 27.7$\\pm$2.8 mJy at 663 MHz). We detect linearly polarized radio emission associated with the `core' and the extended lobes of NGC 4235. Broadband polarimetric analysis yields an RM value of {$\\sim200$ rad m$^{-2}$} in the `core', indicating Faraday rotation by magnetized plasma external to the synchrotron-emitting regions. Using these RM constraints, we estimate an average electron density of the Faraday-rotating medium of $\\sim$3$\\times10^{-2}$ cm$^{-3}$ for a characteristic perturbation scale of $\\sim$0.3 parsec within an assumed magnetized region of size $\\sim$1.3 kpc, consistent with a diffuse magnetized sheath or AGN-driven wind. These results extend classical Faraday rotation diagnostics to the low-power, radio-quiet AGN regime and demonstrate the potential of uGMRT broadband polarimetry for probing magnetized environments in and around such AGN.", "published": "2026-10-07T18:04:58Z", "updated": "2026-10-07T18:04:58Z", "authors": [ "Salmoli Ghosh", "Preeti Kharb", "Janhavi Baghel" ], "url": "https://arxiv.org/abs/2610.10726v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10726", "revision": 1, "status": "ready", "source_fingerprint": "11ddd732985d3124244333ecbf1df6b753babb0f37f1305539f4bd014363f91b", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10726v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10726v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.276Z", "reason": "研究对象是射电宁静 Seyfert 星系的千秒差距尺度射电源及其法拉第旋转介质，与指定的 FRB/PRS 环境、超新星中心引擎或致密天体高能瞬变方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（原文章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Broadband polarimetric analysis yields an RM value of {$\\sim200$ rad m$^{-2}$} in the `core'”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10728", "revision": 1, "title": "Descalarization bursts from Galactic supramassive neutron stars: a kHz continuous-wave target", "abstract": "In massive scalar-tensor gravity, a scalarized neutron star must shed its scalar hair as it collapses into a black hole. Using 3D simulations of a realistic rotating progenitor we show that dispersion stretches the emitted burst into a quasi-monochromatic signal in the kHz frequency range lasting $>10^4$ yr and amenable to continuous-wave methods. We find that detecting these signals in directed searches of supernova remnants without a central pulsar requires sensitivity depths of 233--762 $\\rm{Hz^{-1/2}}$ with the A+-ET-CE detector network. We estimate up to $\\sim3$ of these signals in transit at any observational epoch.", "published": "2026-10-07T18:05:29Z", "updated": "2026-10-07T18:05:29Z", "authors": [ "José Carlos Olvera M.", "Daniela D. Doneva", "Pablo Cerdá-Durán", "José A. Font", "Stoytcho S. Yazadjiev" ], "url": "https://arxiv.org/abs/2610.10728v1", "categories": [ "astro-ph.HE", "gr-qc" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10728", "revision": 1, "status": "ready", "source_fingerprint": "1e65ca4148718563e6ff43b3ab0c104bb487124a8c239fd60fb2a5410bf725f7", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10728v1", "inspected_sections": [ "Introduction", "Supplemental material", "Modeling the supramassive NS progenitor in MSTT.", "Numerical details", "Astrophysical rates", "BH formation by failed CCSN", "Supramassive NS collapse", "Accretion-induced collapse", "Comparison between BH formation channels" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10728v1", "locator": "Introduction; Supplemental material; Modeling the supramassive NS progenitor in MSTT.; Numerical details; Astrophysical rates; BH formation by failed CCSN; Supramassive NS collapse; Accretion-induced collapse; Comparison between BH formation channels", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "be45d247acfdc39745735dbb41df7708790193d5573a782d4237ee88075c7856" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:05:25.049Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "先检查摘要，再按需打开原文。", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “In massive scalar-tensor gravity, a scalarized neutron star must shed its scalar hair as it collapse”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10739", "revision": 1, "title": "Population II Post-AGB Stars. I. Methodology, Initial Results, and the First Luminosity Function", "abstract": "Post-asymptotic giant branch (PAGB) stars share many advantages with the tip of the red giant branch (TRGB) for Population II distance measurements, including minimal internal reddening, easy identification, a solid theoretical foundation, and an expected weak metallicity dependence. At visual wavelengths PAGB stars are the brightest members in old populations, appearing up to $\\sim2$ mag brighter than the TRGB and $\\sim4$ mag brighter than RR Lyrae stars. Stellar evolution theory predicts that these objects occupy a narrow luminosity strip across the top of the Hertzsprung-Russell diagram, making them excellent standard candles. Observations in Galactic globular clusters (GCs) support this prediction, but a comprehensive survey is required to define their luminosity function and test for systematic errors. In this work, we construct a multi-wavelength catalog, spanning the ultraviolet (UV) to infrared (IR), for PAGB stars in 39 Galactic GCs. We validate cluster membership with Gaia astrometry, identify 21 objects across 16 GCs using ground-based uBVI and space-based UV photometry, and perform Bayesian spectral energy distribution (SED) fitting with stellar atmosphere models to estimate their effective temperatures, luminosities, and radii. We find that PAGB stars occupy a narrow luminosity range centered at $\\log(L_{\\mathrm{bol}}/L_{\\odot})=3.25\\pm0.03$, with dispersion $σ=0.12$ dex, supporting their use as reliable Population II distance indicators. Comparisons with theoretical tracks show excellent agreement with evolutionary models. We confirm that PAGB stars occur preferentially in metal-poor clusters with blue horizontal branches. Our results demonstrate that PAGB stars provide a powerful probe of late stellar evolution and a promising Population II standard candle.", "published": "2026-10-07T18:09:14Z", "updated": "2026-10-07T18:09:14Z", "authors": [ "S. Jean Feeser", "Robin Ciardullo", "Michael H. Siegel", "C. J. Hapich", "Akshat S. Chaturvedi" ], "url": "https://arxiv.org/abs/2610.10739v1", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.10739", "revision": 1, "status": "ready", "source_fingerprint": "e766c82b0453ef629ad4a4deb548dc15192be135d59892aec8ef781f75590a06", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10739v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10739v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.277Z", "reason": "论文聚焦球状星团中的后渐近巨星支星及其作为星族 II 标准烛光的用途，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（原文章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “PAGB stars occupy a narrow luminosity range centered at $\\log(L_{\\mathrm{bol}}/L_{\\odot})=3.25\\pm0.03$”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10755", "revision": 1, "title": "Pushing Variability Searches to Extreme Dwarf Galaxies with the Vera C. Rubin Observatory Data Preview 2", "abstract": "Galaxies with stellar masses $M_\\star<10^8~M_\\odot$, hereafter referred to as extreme dwarf galaxies (EDGs), represent one of the least explored regimes in the search for accreting intermediate-mass black holes. Using the recent Vera C. Rubin Observatory Data Preview 2 (DP2; covering 2025-04-25 to 2026-01-06), we present the first systematic search for variability among EDGs in the ELAIS-S1 field, the most extensively observed LSST Deep-Drilling Field in DP2. Applying single-band and cross-band variability statistics to difference-imaging light curves for $6.2\\times10^4$ EDGs with archival multiwavelength characterizations, we identify seven variable EDG candidates, all brighter than $i$-band magnitude of 24 and located within $z<0.3$. The two brightest candidates are previously known AGNs, three have light curves more consistent with supernovae, and two do not have a clear nature. The sample corresponds to an apparent EDG variable fraction of $6.8_{-2.1}^{+3.1}\\times10^{-4}$ at $i$-band magnitudes brighter than 24 and is expected to consist primarily of AGNs and supernovae. Compared to a magnitude-matched massive-galaxy sample with the same variability selection applied, the EDG variable fraction is comparable or at most lower by up to a factor of three. This proof-of-concept study demonstrates that Rubin will identify a statistically meaningful sample of variable EDG candidates, opening a new regime for black-hole demographics. Spectroscopic follow-up will nevertheless be required to secure redshifts and confirm individual candidates.", "published": "2026-10-07T18:22:02Z", "updated": "2026-10-07T18:22:02Z", "authors": [ "Fan Zou", "W. N. Brandt", "Elena Gallo", "Franz E. Bauer", "Angela Bongiorno", "Colin J. Burke", "Alister W. Graham", "Hengxiao Guo", "Lorena Hernández-García", "Marcin Marculewicz", "Dieu D. Nguyen", "Swayamtrupta Panda", "Alessandro Peca", "Bindu Rani", "Claudio Ricci", "Ohad Shemmer", "Wei Leong Tee", "Zhibo Yu" ], "url": "https://arxiv.org/abs/2610.10755v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10755", "revision": 1, "status": "ready", "source_fingerprint": "b0d41909dacdf222056236d3bae2cd95d3d46c19199b269f4301d200383236a4", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10755v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10755v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.277Z", "reason": "论文主要开展极端矮星系中的光学变源搜索，目标是研究中等质量黑洞人口；虽然候选体中包含超新星，但摘要未显示其研究超新星中心引擎或其他指定的高能瞬变问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（原文章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “we identify seven variable EDG candidates, all brighter than $i$-band magnitude of 24 and located within $z<0.3$”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10785", "revision": 1, "title": "The progenitor galaxies of the intracluster light", "abstract": "Intracluster Light (ICL) is a diffuse stellar component of galaxy groups and clusters, bound to the structure's potential rather than to individual galaxies and primarily formed through the stripping and mergers of intermediate-mass galaxies. Its formation and evolution is strongly linked to the central galaxies of groups and clusters, typically the Brightest Cluster Galaxies (BCGs) in clusters. To determine the properties of the progenitor galaxies of the ICL of clusters and groups at redshift z = 0 and compare them with the progenitors of their BCGs. We select 127 clusters and groups in the hydrodynamic Illustris-TNG100 simulation above a mass of 10^{13}~$M_{\\odot}$. We divide the ICL from the BCG by applying a surface brightness cut at the Holmberg radius of 26.5 mag/arcsec^{-2}, where star particles within this radius are defined as attached to the BCG, and outside, the ICL. We then determine the masses and contributions of progenitor galaxies of the ICL and BCG. We find that the number of ICL progenitors increases with structure mass, and that the ICL has more progenitors than the BCG. The ICL has a larger percentage of material from low-mass galaxies. Quenched galaxies contributed a large fraction of the ICL, and this fraction increases with galaxy mass. The mean mass radial gradient of ex-situ material in structures for the ICL and the BCG+ICL is generally negative and increases with structure mass, indicating that material from more massive progenitors is found towards the centres of clusters. The mean mass radial gradient is significantly impacted by structure formation history. ICL progenitor properties are impacted by structure history and are therefore highly individual to each system. At a given structure mass, there is diversity in the properties of the progenitors that formed the ICL. Although the BCG and the ICL co-evolve, the BCG has fewer, more massive progenitors.", "published": "2026-10-07T18:43:16Z", "updated": "2026-10-07T18:43:16Z", "authors": [ "Rebecca J. Mayes", "Facundo A. Gómez", "Antonela Monachesi" ], "url": "https://arxiv.org/abs/2610.10785v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10785", "revision": 1, "status": "ready", "source_fingerprint": "540d8aaaebb5c33da73a814d6345c6e0dae90ec7be7e34ba7da8f6872442f22d", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10785v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10785v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.277Z", "reason": "论文研究星系团内星光的起源及其前身星系，与高能瞬变、致密天体观测或相关辐射环境无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Intracluster Light (ICL) is a diffuse stellar component of galaxy groups and clusters, bound to the”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10815", "revision": 1, "title": "Shortening the Baseline: Characterising Type Ia Supernovae Using $Δm_{10}(X)$", "abstract": "An explorative study of Type Ia Supernovae (SNe Ia) light curves is presented. $Δm_{t}(X)$ decline-rate metrics are used to evaluate alternative characterisations of light curve diversity and the Luminosity-Width Relation (LWR). Using a sample of 362 SNe Ia from the Carnegie Supernova Project (CSP-I and CSP-II), Gaussian Process regression is used to fit $B$- and $g$-band light curves and measure decline-rates across multiple post-maximum timescales. The LWR is calibrated using a clean subsample of SNe Ia with host-independent distance moduli and Fitzpatrick (1999) reddening corrections. Decline-rates $Δm_{10}(B)$ and $Δm_{10}(g)$ are found to capture the LWR effectively, while mitigating the severe degeneracy that affects longer timescales for fast-declining ($Δm_{15}(B) \\geq 1.6$ mag) events. Continuous, piecewise linear models are presented that seamlessly anchor the transition between normal and fast-declining regimes. The decline-rate $Δm_{10}(X)$ closely approximates the results of the more complex colour-stretch parameters, requiring less post-maximum temporal coverage than $Δm_{15}(B)$ or $s_{BV}$, and offers an even greater sensitivity for slow decliners. $Δm_{10}(B)$ provides a precise and practical tool for large-scale photometric surveys and real-time observer classification.photometric surveys and real-time observer classification.", "published": "2026-10-07T19:19:02Z", "updated": "2026-10-07T19:19:02Z", "authors": [ "Joel M. Velasco", "Paolo A. Mazzali", "Christopher Ashall", "Christopher R. Burns", "Mark M. Phillips", "Lluis Galbany", "Nidia Morrell", "Maximilian D. Stritzinger", "Peter Hoeflich", "Eric Y. Hsiao", "Syed A. Uddin" ], "url": "https://arxiv.org/abs/2610.10815v1", "categories": [ "astro-ph.HE", "astro-ph.SR" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.10815", "revision": 1, "status": "ready", "source_fingerprint": "540ababc706653be3bd955c0c1b607e826c0022cdc4bc7facb2ae170341057e1", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10815v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10815v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.278Z", "reason": "论文讨论 Ia 型超新星的光变衰减率与光度—宽度关系，但摘要未涉及中心引擎、平台期、激波破越或周星介质相互作用等目标问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The LWR is calibrated using a clean subsample of SNe Ia with host-independent distance moduli and Fitzpatrick (1999) reddening corrections.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10866", "revision": 1, "title": "Observational Signatures of Dyonic Black Holes in Non-Linear Electrodynamics", "abstract": "We study the observational features of thin-disk accretion and emission spectra for static, spherically symmetric dyonic black holes in non-linear electrodynamics (NLED). In contrast to classical Maxwell theory, where electromagnetic duality assumes equal charges, the coupling parameters in NLED introduce a new gravitational potential and modify the geometry in the strong-field regime. We also study the kinematic characteristics of particles on circular orbits, such as their angular velocity, specific energy, and specific angular momentum. It is found that modifications of NLED lead to a shrinkage of the ISCO radius, resulting in a shift of the radiation spectrum thermal maximum towards smaller radii and, consequently, an increase in the local effective temperature in comparison with the standard Schwarzschild and Reissner-Nordström solutions. Additionally, we compute null-geodesic orbits to determine the optical edge of both the photon sphere and the black hole shadow. In order to assess the observational validity of the aforementioned alternatives, we carry out a $χ^2$ goodness-of-fit test through the angular diameter constraints at the horizon scale collected by the Event Horizon Telescope (EHT) concerning Sagittarius A* ($\\text{Sgr A}^*$). We prove that both these dyonic NLED and purely magnetic models have good statistical agreement with experimental data.", "published": "2026-10-07T20:11:38Z", "updated": "2026-10-07T20:11:38Z", "authors": [ "Sobhan Kazempour", "Sichun Sun", "Zhiqing He", "Chengye Yu" ], "url": "https://arxiv.org/abs/2610.10866v1", "categories": [ "gr-qc", "astro-ph.HE", "hep-ph" ], "primary_category": "gr-qc", "analysis": { "arxiv_id": "2610.10866", "revision": 1, "status": "ready", "source_fingerprint": "639a8e214597cae8b24f0aff38973827d3f0f9f38a127b9924ba69cbb97de4e4", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.10866v1", "inspected_sections": [ "I Introduction", "II The Dyonic Black Hole Metric in Non-Linear Electrodynamics", "III Geodesic Motion and Fundamental Orbital Dynamics", "III.1 The Magnetic Black Hole", "IV Physics of the Thin Accretion Disk", "IV.1 The Magnetic Black Hole", "V Numerical Analysis", "V.1 Observable Signatures and Astrophysical Implications", "V.1.1 Thermal Spectrum and Radiative Efficiency", "V.1.2 The Photon Sphere and Black Hole Shadow", "V.2 The Magnetic Black Hole", "VI Conclusions" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.10866v1", "locator": "I Introduction; II The Dyonic Black Hole Metric in Non-Linear Electrodynamics; III Geodesic Motion and Fundamental Orbital Dynamics; III.1 The Magnetic Black Hole; IV Physics of the Thin Accretion Disk; IV.1 The Magnetic Black Hole; V Numerical Analysis; V.1 Observable Signatures and Astrophysical Implications; V.1.1 Thermal Spectrum and Radiative Efficiency; V.1.2 The Photon Sphere and Black Hole Shadow; V.2 The Magnetic Black Hole; VI Conclusions", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "0cd7e249cdd6983f6e108de8379afd4ef52374499109051ba2ce3b7280f5596f" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:32:19.231Z", "reason": "该论文研究非线性电动力学（NLED）框架下的静态双荷（dyonic）黑洞时空度规、最内稳定圆轨道（ISCO）、薄吸积盘热辐射特征及黑洞阴影尺寸，属于修正引力与理论高能物理度规计算，与高能瞬变天体物理组所关注的 FRB/PRS 及其环境、超新星中心引擎、激波破越与周星相互作用、相对论喷流及高能中微子等无实质联系。", "result": "通过度规函数求解与测地线分析表明，双荷与纯磁荷使 ISCO 半径向内收缩（例如 Magnetic 2 模型收缩至 $\\bar{r}_{\\rm ISCO}=4.891$），吸积盘辐射通量峰值与辐射效率显著提高（最高可达 $\\eta = 1 - \\bar{E}_{\\rm ISCO} \\approx 6.90\\%$，高于标准 Schwarzschild 的 $5.72\\%$）；利用 Sgr A* 质量与距离导出的黑洞阴影角直径（$\\theta \\approx 45.32\\text{--}51.72\\,\\mu\\mathrm{as}$）均落在 EHT $1\\sigma$ 至 $2\\sigma$ 限制内（$\\chi^2 < 1$）。", "reading_entry": "II The Dyonic Black Hole Metric in Non-Linear Electrodynamics", "problem": "研究在非线性电动力学（NLED）修正下，破坏线性麦克斯韦电磁对偶性的双荷（dyonic，兼具电荷 $q$ 与磁荷 $p$）黑洞度规结构，探讨其对吸积盘辐射特征与事件视界望远镜（EHT）黑洞阴影观测的潜在影响及可区分度。", "method": "求解包含非线性电磁耦合项 $a, b$ 的球对称度规函数 $f(r)$，利用有效势二阶导数判据 $\\frac{\\mathrm{d}^2 \\bar{V}_{\\rm eff}}{\\mathrm{d}\\bar{r}^2}=0$ 确定 ISCO 半径，基于 Novikov-Thorne 几何薄盘模型积分计算能量通量 $F(r)=\\frac{-\\dot{M}_{0}}{4\\pi\\sqrt{-g}}\\frac{\\bar{\\Omega}_{,r}}{(\\bar{E}-\\bar{\\Omega}\\bar{L})^{2}}\\int_{r_{\\rm ISCO}}^{r}(\\bar{E}-\\bar{\\Omega}\\bar{L})\\bar{L}_{,r}\\mathrm{d}r$，并结合光子球半径 $\\bar{r}_{\\rm ph}$ 计算阴影临界碰撞参数 $\\bar{b}_{\\rm crit}$ 与天球角直径 $\\theta$ 进行 EHT 数据 $\\chi^2$ 拟合。", "assumptions": [], "limits": [], "citation_leads": [ "II The Dyonic Black Hole Metric in Non-Linear Electrodynamics: “The Dyonic Black Hole Metric in Non-Linear Electrodynamics”", "IV Physics of the Thin Accretion Disk: “Physics of the Thin Accretion Disk”", "V.1.2 The Photon Sphere and Black Hole Shadow: “The Photon Sphere and Black Hole Shadow”" ], "research_progress": "明确了 NLED 耦合项在度规函数中诱发的 $r^{-6}$ 阶修正项对黑洞有效势垒、吸积盘有效温度剖面 $T(r) \\propto r^{-3/4}$ 与辐射效率 $\\eta$ 的理论调控规律，并给出了 Sgr A* 阴影角直径对 NLED 参数的统计约束上限。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10901", "revision": 1, "title": "Mass Proxy Quality of Halo Properties in IllustrisTNG and FLAMINGO Simulations: II. Galaxies, Stars, and Black Holes", "abstract": "We study the stellar, black hole, and satellite galaxy populations of group- and cluster-scale halos in the IllustrisTNG, TNG-Cluster, and FLAMINGO cosmological hydrodynamical simulations. We characterize the mass-conditioned scaling relations, covariance, conditional likelihoods, and mass proxy quality (MPQ) of integral properties within $R_{\\rm 500c}$: total stellar mass ($M_{\\star,\\,\\rm tot}$), brightest central galaxy stellar mass ($M_{\\star,\\,\\rm BCG}$), intracluster light mass ($M_{\\star,\\,\\rm ICL}$), total black hole mass ($M_{\\rm BH}$), satellite occupation ($N_{\\rm sat}$), and satellite velocity dispersion ($σ_{\\rm sat,\\,1D}$), at $z\\in \\{0,0.5,1,2\\}$. While normalization differences of up to a factor of two emerge among simulations, many properties exhibit remarkably similar mass-localized slopes, intrinsic scatters, and MPQs across halo samples and redshifts. Correlations among stellar, satellite, and gas properties are generally consistent in sign and their dependence on halo mass and redshift, whereas those involving $M_{\\rm BH}$ and $N_{\\rm sat}$ show greater variation, particularly in TNG-Cluster. Conditional likelihoods are nearly lognormal for many properties, including $M_{\\star,\\,\\rm tot}$, $N_{\\rm sat}$, and $σ_{\\rm sat,\\,1D}$, while $M_{\\star,\\,\\rm BCG}$ and $M_{\\star,\\,\\rm ICL}$ are negatively skewed. Among the properties considered here, total stellar mass is the best mass proxy, with a halo mass scatter of $7$-$14\\%$, followed by $N_{\\rm sat}$ with a mass scatter of $9$-$18\\%$. The consistent correlation behavior of $M_{\\star,\\,\\rm ICL}$ highlights its potential for next-generation observational studies. Finally, $σ_{\\rm sat,\\,1D}$ exhibits highly consistent scaling, with mass-independent slope and scatter and a largely neutral correlation structure, suggesting that it is relatively insensitive to astrophysical complexity.", "published": "2026-10-07T20:58:26Z", "updated": "2026-10-07T20:58:26Z", "authors": [ "Eddie Aljamal", "August E. Evrard", "Arya Farahi", "Dylan Nelson" ], "url": "https://arxiv.org/abs/2610.10901v1", "categories": [ "astro-ph.GA", "astro-ph.CO" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10901", "revision": 1, "status": "ready", "source_fingerprint": "3fff4366cdb153c0f2e6cb9713da7d030a2326bdf138542879a29b346026cdb5", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10901v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10901v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.278Z", "reason": "论文比较星系团尺度晕的星系、恒星和黑洞群体及质量代理性质，属于大尺度结构与星系形成研究，与目标高能瞬变方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We study the stellar, black hole, and satellite galaxy populations of group- and cluster-scale halos in the IllustrisTNG, TNG-Cluster, and FLAMINGO cosmological hydrodynamical simulations.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10910", "revision": 1, "title": "Understanding how Coronal Heating and Magnetic Field Scaling Affect Global Properties of the Low and Middle Corona", "abstract": "The magnetic field of the Sun is a key driver of coronal heating and solar wind acceleration. In tandem, these influence the observable morphology of the corona, along with defining the magnetic connectivity and magnitude of open magnetic flux. Here,we investigate how coronal heating affects the magnetothermal state of the 3D global corona by analyzing a series of data-constrained, thermodynamic magnetohydrodynamic (MHD) simulations for solar minimum conditions. We vary the overall heat deposited in the corona via modifying the input Poynting flux of a wave-turbulence-driven (WTD) model for coronal heating and by scaling the inner boundary magnetic field. We quantify the magnetic, thermodynamic, and combined magnetothermal effects on our simulations. We find that increasing the overall amount of heat leads to a higher magnitude of open flux and a more visibly open white-light morphology in the K-Corona between 1.5 and 6 Rsun. We quantify how plasma beta evolves and drives morphological differences between simulations. We also compare these runs to an extremely high-resolution reference solution that includes small-scale magnetic information in the surface boundary condition. This latter comparison provides insight into the further development of 'subgrid' corrections for low(er) resolution models to best represent the structure and observables of the corona and inner heliosphere.", "published": "2026-10-07T21:07:49Z", "updated": "2026-10-07T21:07:49Z", "authors": [ "Caroline L. Evans", "Cooper Downs", "Donald Schmit" ], "url": "https://arxiv.org/abs/2610.10910v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.10910", "revision": 1, "status": "ready", "source_fingerprint": "d38e325f6f3653213f07e3d04ead8609c302f44c57571a0bdb4cb1d4978e16e0", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10910v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10910v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.278Z", "reason": "研究太阳日冕加热、太阳风及日冕磁场形态，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The magnetic field of the Sun is a key driver of coronal heating and solar wind acceleration.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10936", "revision": 1, "title": "The conditional colour-magnitude distribution: III. A study of galaxy colour- and luminosity-dependent counts-in-cells statistics", "abstract": "The conditional colour-magnitude distribution (CCMD) model connects the galaxy colour-luminosity distribution with dark matter halo mass, which has been constrained in Xu et al. by jointly modelling the two-point correlation functions of a large galaxy sample of the Sloan Digital Sky Survey (SDSS) in fine bins of galaxy colour and luminosity. We test the CCMD model of the galaxy-halo connection using counts-in-cells (CIC) statistics by comparing CCMD model predictions with SDSS measurements for 16 subsamples of galaxies in various luminosity and colour bins. In addition, we compare SDSS measurements with three analytic models of CIC distribution. The CCMD model provides a good description of the SDSS CIC measurements for most subsamples. The exceptions are the void probability functions and CIC distributions with cell radius 5 Mpc/h for a few subsamples in the luminous bins, which are not well described by the analytic models, either. For these subsamples, in general, removing the Sloan Great Wall from SDSS or introducing velocity bias to the CCMD model does not resolve the disagreement. Finally, with the help of the CCMD mocks, we investigate the cause of the variations of the galaxy counts in cells. For small cells or cells with a low mean galaxy count, the variation reflects effects from fluctuations in both the matter environment and the halo occupation distribution, while for large cells or cells with a high mean galaxy count, the environment effect dominates. We discuss the implications of our work for investigating galaxy assembly bias.", "published": "2026-10-07T21:42:43Z", "updated": "2026-10-07T21:42:43Z", "authors": [ "Raymon Isaac", "Zheng Zheng" ], "url": "https://arxiv.org/abs/2610.10936v1", "categories": [ "astro-ph.GA", "astro-ph.CO" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10936", "revision": 1, "status": "ready", "source_fingerprint": "ff2d6a13d914536042d82c353411a9318102567291d6c0ca974fcea59fee9fa2", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10936v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10936v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.279Z", "reason": "论文研究星系颜色—光度分布、暗物质晕及 counts-in-cells 统计，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We test the CCMD model of the galaxy-halo connection using counts-in-cells (CIC) statistics”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.10941", "revision": 1, "title": "Central stellar depletion in the Draco dwarf from Subaru photometry", "abstract": "Dark matter subhaloes are a fundamental prediction of the standard cosmological model, but their low-mass population remains difficult to constrain observationally. Recent work has shown that interactions between subhaloes and dwarf spheroidal galaxies can induce large-scale, out-of-equilibrium fluctuations in their stellar surface density fields, identifiable through Fourier-based statistics. We apply this formalism to deep Subaru photometry of the Draco dwarf, extending previous tests to $\\gtrsim\\mathcal{O}(10^{4})$ resolved stars. We use artificial-star tests to assign completeness weights to individual stars and incorporate them into a discrete likelihood-based framework. Relative to a cored axisymmetric Plummer model, Draco shows radial corrugations that appear in the filtered normalised residuals as a central stellar depletion surrounded by a ring-like excess. The same feature appears in Fourier space as a low-frequency peak with a signal-to-noise ratio ${\\rm S/N}=6.0$. Independently, fitting the surface density $Σ$ with an $αβγ$ model yields ${\\rm d}Σ/{\\rm d}R>0$ at $>99.9\\%$ confidence -- i.e., a profile that decreases towards the centre. Although these signatures cannot yet be regarded as robust evidence for dark subhaloes, they suggest that central stellar depletion in dwarf galaxies may reflect genuine physical structure rather than crowding alone.", "published": "2026-10-07T21:45:24Z", "updated": "2026-10-07T21:45:24Z", "authors": [ "Eduardo Vitral", "Kyosuke S. Sato", "Jorge Peñarrubia", "Sakurako Okamoto", "Veronika Dornan" ], "url": "https://arxiv.org/abs/2610.10941v1", "categories": [ "astro-ph.GA", "astro-ph.IM" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.10941", "revision": 1, "status": "ready", "source_fingerprint": "c5448f8b8eaf7a78781e6e3c1640285db6b2078e3394ebb37f3a22566924fe58", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.10941v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.10941v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.279Z", "reason": "论文研究矮星系 Draco 的恒星表面密度结构及暗物质子晕线索，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Draco shows radial corrugations that appear in the filtered normalised residuals as a central stellar depletion surrounded by a ring-like excess.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11016", "revision": 1, "title": "NGC 6426: Colour-Magnitude diagram and variable star population as indicators of metallicity, distance, and age", "abstract": "We present new VI CCD photometry of the globular cluster NGC 6426. The membership status of all point sources and, in particular, of all the variables in the field of view is discussed, including four recently detected variables. The double mode nature of variables V3 and V9 is confirmed and their periods are calculated. The presence of a cluster member anomalous Cepheid (V17) is reported. Employing only likely members we produce a decontaminated colour-magnitude diagram (CMD) differentially dereddened, which enables us to compare it with theoretical predictions and to study the variable stars distribution. The mean cluster metallicity and distance were calculated via the RR Lyrae V-band light curve Fourier decomposition and an I-band calibration of the Period-Magnitude-Metallicity relation. Further, a comparison using a Bayesian approach between theoretical isochrones of Dartmouth Stellar Evolution Database (DSED), with a deep HST CMD, gave us independent estimates of distance modulus, metallicity, colour excess, and cluster age.", "published": "2026-10-07T23:55:37Z", "updated": "2026-10-07T23:55:37Z", "authors": [ "A. Arellano Ferro", "R. Michel", "D. Deras", "M. Vaca Montejano", "S. Muneer", "I. Bustos Fierro" ], "url": "https://arxiv.org/abs/2610.11016v1", "categories": [ "astro-ph.GA", "astro-ph.SR" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.11016", "revision": 1, "status": "ready", "source_fingerprint": "eb61ce51a58700b4e57d53477cde47ba3600c316a8dafddff3d78ee878589ef2", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11016v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11016v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.279Z", "reason": "论文研究球状星团的色—星等图、变星及其金属丰度、距离和年龄，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The mean cluster metallicity and distance were calculated via the RR Lyrae V-band light curve Fourier decomposition”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11091", "revision": 1, "title": "Systematic Uncertainties in Ultralight Boson Constraints from Superradiance", "abstract": "Ultralight bosons are well-motivated candidates for physics beyond the Standard Model and may constitute part or all of the dark matter. Black-hole superradiance provides a powerful means of probing these particles through their gravitational interaction with rotating black holes. This mechanism has motivated a growing body of constraints from electromagnetic measurements of black-hole spins and, more recently, gravitational-wave observations. Gravitational-wave probes draw on several distinct signatures: the spins of merging binary black holes, gravitational radiation emitted by boson clouds, and potential imprints of cloud-induced changes to binary dynamics. The interpretation of these probes depends on method-specific astrophysical and theoretical assumptions, including black hole formation, natal spin, age, accretion history, population priors, and boson self-interactions. In this paper, we review the principal electromagnetic and gravitational-wave constraints derived from black-hole superradiance, with particular emphasis on their underlying assumptions and systematic uncertainties. The distinct observational signatures and systematic uncertainties of these approaches offer complementary perspectives on the viability of ultralight-boson models. In particular, their overlapping coverage around boson masses of $10^{-13}$-$10^{-12}$ eV makes this region particularly informative for comparing constraints, with attention to the assumptions underlying each result.", "published": "2026-10-08T02:04:48Z", "updated": "2026-10-08T02:04:48Z", "authors": [ "P. S. Aswathi", "Ling Sun" ], "url": "https://arxiv.org/abs/2610.11091v1", "categories": [ "hep-ph", "astro-ph.HE" ], "primary_category": "hep-ph", "analysis": { "arxiv_id": "2610.11091", "revision": 1, "status": "ready", "source_fingerprint": "89b9523833b61756ec3e4f48648b9f54b0c367b9649553c14006ae5dd3a0db11", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11091v1", "inspected_sections": [ "Introduction", "Constraints from electromagnetic observations labelsec:EM_observations_constraints", "Constraints from black-hole spins inferred from gravitational-wave observationslabelsec:GW_spin_constraints", "Gravitational-wave searches for boson clouds", "Self-interactions and non-gravitational couplings", "Conclusions", "Reference table for Figure~reffig:superradiance_constraints" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11091v1", "locator": "Introduction; Constraints from electromagnetic observations labelsec:EM_observations_constraints; Constraints from black-hole spins inferred from gravitational-wave observationslabelsec:GW_spin_constraints; Gravitational-wave searches for boson clouds; Self-interactions and non-gravitational couplings; Conclusions; Reference table for Figure~reffig:superradiance_constraints", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "2bb0eed809c5f3cd907d0b90ac31a01e3a8845ee19641cd004ed449935789b56" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:08:01.367Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "先检查摘要，再按需打开原文。", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “Ultralight bosons are well-motivated candidates for physics beyond the Standard Model and may consti”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11095", "revision": 1, "title": "Production Memory of the $^{225}\\mathrm{Ra}$-$^{225}\\mathrm{Ac}$ Clock in Neutron-Star Merger Ejecta", "abstract": "Radioactive nuclei in neutron-star merger ejecta carry information about both their abundance and their production history. Using the $^{225}\\mathrm{Ra}$-$^{225}\\mathrm{Ac}$ sequence, we establish exact conditions linking a surviving isotope partition to the time available for parent decay. An Ac fraction of 0.1 produced solely through Ra decay requires at least 2.456 days, providing a direct consistency test for proposed source states. We show that subsequent activity retains additional production memory: two histories with the same mean birth time can produce different response crossings. This distinction is captured analytically and separates mean chronology from the influence of the production-time distribution. A controlled radiation calculation then shows how deposition and photon escape transform the nuclear contrast into a common light-curve pivot for fixed ejecta properties. The results connect nuclear production chronology to late-time merger emission and provide benchmarks for nucleosynthesis and radiation-transport calculations.", "published": "2026-10-08T02:11:20Z", "updated": "2026-10-08T02:11:20Z", "authors": [ "Hisham Anwer" ], "url": "https://arxiv.org/abs/2610.11095v1", "categories": [ "nucl-th", "astro-ph.HE" ], "primary_category": "nucl-th", "analysis": { "arxiv_id": "2610.11095", "revision": 1, "status": "ready", "source_fingerprint": "3b8c002932fb2ac7d716ba473b8a5214370bb4ea124b63894a6a250186187651", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11095v1", "inspected_sections": [ "The source history of a late radioactive clock", "Accessible source states and exact timing identities", "From controlled source states to photons", "Physical checks and observational conditioning", "Conclusion" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11095v1", "locator": "The source history of a late radioactive clock; Accessible source states and exact timing identities; From controlled source states to photons; Physical checks and observational conditioning; Conclusion", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "83c05b7a6c243e1f7ef0e9ff4afe8630b05d8da9f5a37b0e90ef0da4050b2841" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:08:08.317Z", "reason": "本研究专注于双中子星并合抛射物中 $^{225}\\mathrm{Ra}$-$^{225}\\mathrm{Ac}$ 衰变链的核反应产生历史、带电粒子能量沉积及晚期千新星灰体光度演化，不涉及 FRB/PRS、超新星中心引擎、激波破越与 CSM 相互作用、相对论喷流、中微子探测或高能观测等本组核心关注方向。", "result": "推导出了纯 Ra 衰变通道下 Ac 存活分额的精确反演最小时间下限公式：$$T_{\\min}(p) = -\\frac{1}{\\lambda_{\\rm Ac}-\\lambda_{\\rm Ra}} \\ln\\left[1 - \\frac{\\lambda_{\\rm Ac}-\\lambda_{\\rm Ra}}{\\lambda_{\\rm Ra}} \\frac{p}{1-p}\\right]$$ 对于采用的衰变常数，达到 $p=0.1$ 的 Ac 分额至少需要 $T_{\\min} \\ge 2.45594\\;\\mathrm{d}$；对任意核产生分布 $g(u)$，给出了产额注入后期的特征反转零点表达式：$$t_g = t_n + \\frac{K_g(\\lambda_{\\rm Ac})-K_g(\\lambda_{\\rm Ra})}{\\lambda_{\\rm Ac}-\\lambda_{\\rm Ra}} \\approx t_n + \\mu + \\frac{\\lambda_{\\rm Ac}+\\lambda_{\\rm Ra}}{2}\\sigma^2 + O(\\epsilon^3)$$ 其中纯脉冲交叉时刻为 $t_n = 17.4942\\;\\mathrm{d}$，方差 $\\sigma^2$ 提供一阶正修正。结合粒子热化与灰体光子扩散计算后，光子交叉时刻被推迟至 $25.592\\;\\mathrm{d}$，且在固定转移条件下所有分额共享一个无依赖的光变交汇枢纽点（pivot）。", "reading_entry": "Accessible source states and exact timing identities", "problem": "在双中子星并合抛射物中，晚期快中子俘获过程同位素产额与母核衰变历史之间存在简并，如何从核衰变链时序中提取放射性母核的产生历程，并确定粒子能量沉积与光子扩散如何改变晚期光变观测特征。", "method": "利用两阶段 Bateman 方程结合生成函数与累积量展开（cumulant expansion）推导活度矩与交叉时标解析解；采用 Hotokezaka & Nakar (2020) 处方进行多成分粒子能量沉积计算，并结合球对称同源膨胀抛射物（密度 $\\rho \\propto t^{-3}v^{-4.5}$）的灰体扩散模型追踪辐射逃逸，计算差分光度响应 $L_{p_1}-L_{p_0}=Y_{225}(p_1-p_0)(G_A-G_U)$。", "assumptions": [], "limits": [], "citation_leads": [ "The source history of a late radioactive clock: “Late-time kilonova emission connects the heavy nuclei synthesized in neutron-star mergers to their radioactive histories”", "The source history of a late radioactive clock: “Interpreting this sequence requires both abundance and production chronology.”", "Accessible source states and exact timing identities: “A fraction $p=0.1$ requires 2.45594 d; an earlier reference state therefore requires independent Ac production”", "Accessible source states and exact timing identities: “In the two-stage approximation every Ra decay feeds Ac, and Ac decay removes a nucleus from the counted pair.”", "Accessible source states and exact timing identities: “Convolution gives the post-feed activity contrast”", "Accessible source states and exact timing identities: “The positive leading variance correction shifts the crossing beyond the mean-shifted impulse anchor”", "From controlled source states to photons: “homologous density $\\rho(v,t)\\propto t^{-3}v^{-4.5}$ normalized to $M$, outer/inner gray opacities $(0.5,3.0)$ cm$^2$ g$^{-1}$”", "Physical checks and observational conditioning: “These fixed groups model escape-time variation without frequency redistribution or temperature-dependent opacity.”", "Physical checks and observational conditioning: “These model perturbations and precision benchmarks have no assigned astrophysical population probability.”" ], "research_progress": "建立了利用 $^{225}\\mathrm{Ra}$-$^{225}\\mathrm{Ac}$ 衰变时钟约束核合成历史的解析判据与存活分额年龄下限，明确将均值时序与产生历程高阶矩（如方差）的影响在活度交叉特征中解耦，并定量给出了辐射扩散对该特征时间引入的约 8 天时延标定。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11102", "revision": 1, "title": "The Binary Fraction of Milky Way Field Stars in DESI: Dependence on Chemical Abundance", "abstract": "Binary populations encode information about the physical conditions of star formation and the subsequent evolution of stellar populations. Adopting a statistical method based on multi-epoch line-of-sight velocity variations, we constrain the binary fraction, $f_b$, of field main-sequence turn-off stars in the Milky Way using data from the second data release of the DESI Milky Way Survey. $f_b$ is found to primarily increase with lower [Fe/H]. At $[\\mathrm{Fe}/\\mathrm{H}]\\gtrsim -1.3$, $f_b$ shows a modest increase with increasing [Mg/Fe], whereas no clear trend is detected at lower [Fe/H]. The apparent variations of $f_b$ with angular momentum and Galactic height are largely explained by their underlying [Fe/H] distributions, while the remaining variations broadly follow differences in [Mg/Fe]. Within overlapping regions of the [Fe/H]--[Mg/Fe] plane, the thin disk, thick disk, stellar halo and GSE populations exhibit no significant differences in their binary fractions. Thus, our measurements indicate that the variation in $f_b$ is dominated by chemical abundance, which could be explained by the metallicity-dependent gas cooling efficiency and fragmentation. The weaker [Mg/Fe] dependence at fixed [Fe/H] might be associated with the formation conditions of stars, with higher [Mg/Fe] stars generally forming earlier under a more gas-rich and turbulent environment.", "published": "2026-10-08T02:19:07Z", "updated": "2026-10-08T02:19:07Z", "authors": [ "Tian Qiu", "Wenting Wang", "Sergey E. Koposov", "Songting Li", "Nathan Sandford", "Ting S. Li", "Joan Najita", "Jessica Nicole Aguilar", "Steven Ahlen", "Davide Bianchi", "David Brooks", "Aurelio Carnero Rosell", "Todd Claybaugh", "Andrei Cuceu", "Axel de la Macorra", "Arjun Dey", "Peter Doel", "Jaime E. Forero-Romero", "Enrique Gaztañaga", "Satya Gontcho A Gontcho", "Gaston Gutierrez", "Stephanie Juneau", "Robert Kehoe", "Martin Landriau", "Laurent Le Guillou", "Aaron Meisner", "Ramon Miquel", "Enrique Paillas", "Will Percival", "Francisco Prada", "Ignasi Pérez-Ràfols", "Corentin Ravoux", "Graziano Rossi", "Eusebio Sanchez", "Christoph Saulder", "Edward Schlafly", "David Schlegel", "Michael Schubnell", "Joseph Harry Silber", "Małgorzata Siudek", "Gregory Tarlé", "Benjamin Alan Weaver" ], "url": "https://arxiv.org/abs/2610.11102v1", "categories": [ "astro-ph.GA", "astro-ph.SR" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.11102", "revision": 1, "status": "ready", "source_fingerprint": "da24e72ca82f53df03ea03c59f64122f1a9406961ec5610492d0074160045dcb", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11102v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11102v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.279Z", "reason": "论文研究银河系场星的双星比例及其与化学丰度的关系，摘要未涉及指定的高能瞬变、致密天体高能观测或相关环境问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Thus, our measurements indicate that the variation in $f_b$ is dominated by chemical abundance”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11127", "revision": 1, "title": "Improved analysis of time delays between radio wavelengths and X-ray of Sgr A* flares in the shock oscillation model", "abstract": "We present an improved analysis of the time delays between radio and X-ray flares from the supermassive black hole Sagittarius A* (Sgr A*), extending our previous shock oscillation model by incorporating Compton scattering. Our simulations predict delay times of 1-4 h between X-ray and radio flares, 20-40 min and 0.5-1 h between 334 GHz and 4.5 $μ$m and 2-8 keV flares, and 7-20 min and 0.5-1 h between 22-43 GHz and 350 GHz radio flares, respectively, in good agreement with recent observations. The delay time between the radio emissions (synchrotron) and X-ray emissions (bremsstrahlung) is interpreted as the transit time for sound waves traveling from the central core near the event horizon to the location of the oscillating shock. Additionally, the delay time observed between different radio wavelengths corresponds to the transit time of sound waves moving between the frequency-dependent effective radii $R_{\\rm eff}(ν)$, where the optical thickness $τ_ν(R)$ at frequency $ν$ equals one on the surface of the accretion disc. The X-ray emission and the radio emission at lower frequencies peak later than the radio emission at higher frequencies. This delay occurs because the acoustic perturbations created by synchrotron emission peak near the event horizon and then expand outward. Conversely, an inverse delay happens when the acoustic waves generated by the upstream shock wave travel toward the event horizon. The predicted delay times from this interpretation qualitatively match the numerical results obtained in simulations.", "published": "2026-10-08T02:53:14Z", "updated": "2026-10-08T02:53:14Z", "authors": [ "Ramiz Aktar", "Toru Okuda", "Chandra B. Singh" ], "url": "https://arxiv.org/abs/2610.11127v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11127", "revision": 1, "status": "ready", "source_fingerprint": "7180b43e6b01e583604cc6b0b52bbb7b7c044febee92cd1aad8e04a15db5373a", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11127v1", "inspected_sections": [ "Introduction", "2 NUMERICAL METHOD" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11127v1", "locator": "Introduction; 2 NUMERICAL METHOD", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "8dc1c47ad93e5c5214d6eb5cea47210fc2084d33d66b2cd4db9076ea280e1fa0" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:10:27.245Z", "reason": "已检查材料没有提供可核验的说明。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "Introduction", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Introduction: “We present an improved analysis of the time delays between radio and X-ray flares from the supermass”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11166", "revision": 1, "title": "Analysis of p-Wave Sommerfeld Resonance Behavior in Finite-Size Dark Matter", "abstract": "Different stages of cosmic evolution impose different requirements on the dark matter annihilation cross section. Sommerfeld enhancement provides a possible way to accommodate them. However, in the point-like dark matter scenario, satisfying these requirements with either $s$-wave or $p$-wave Sommerfeld enhancement can strongly constrain the dark matter and mediator masses and their coupling. A finite dark matter size introduces an additional parameter and may relax these constraints. Motivated by this possibility, in this work we study the $p$-wave Sommerfeld resonances of finite-size dark matter (like proton or neutron) without specifying its internal structure. We find that the $p$-wave contribution can exceed the $s$-wave contribution. Nevertheless, the finite-size $p$-wave resonances are weaker than those in the point-like case. Despite this suppression, their velocity dependence remains similar to that of point-like dark matter. We then extend our analysis to nugget dark matter composed of a small number of constituents. In this case, the $p$-wave Sommerfeld enhancement exhibits behavior similar to that of point-like dark matter.", "published": "2026-10-08T03:24:39Z", "updated": "2026-10-08T03:24:39Z", "authors": [ "Wu-Long Xu", "Jin Min Yang", "Rui Zhu" ], "url": "https://arxiv.org/abs/2610.11166v1", "categories": [ "hep-ph", "astro-ph.HE", "hep-th" ], "primary_category": "hep-ph", "analysis": { "arxiv_id": "2610.11166", "revision": 1, "status": "ready", "source_fingerprint": "436ca274debc9a86623cece68176f241baf56d212e50dfcd00ce5d320249091d", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11166v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11166v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.280Z", "reason": "论文研究有限尺寸暗物质的 p 波 Sommerfeld 共振，虽有 astro-ph.HE 分类，但摘要未显示其与 FRB、超新星、激波、相对论喷流、中微子或致密天体高能观测有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（实际章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “we study the $p$-wave Sommerfeld resonances of finite-size dark matter”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11182", "revision": 1, "title": "Direct Numerical Comparison of Data Driving Strategies for Solar Flux Emergence in Magnetohydrodynamics: B-driving vs E-driving", "abstract": "Data driving is an important technique for modelling realistic magnetic field and plasma evolution in regions of the solar atmosphere where direct observations are either absent or insufficient. This technique uses observational data to drive the evolution of the simulation, while the modelled solar atmosphere evolves self-consistently. A common approach for data-driven simulations is B-driving, which uses the observed magnetic field at the surface of the Sun as a boundary condition. However, only prescribing B at the boundary does not generally determine its numerical evolution when the update depends on the reconstructed interface states or fluxes. To address this, E-driving provides an alternative approach by instead driving the simulation using the electric field on the boundary, which directly controls the magnetic field update. We systematically quantify the performance of B- and E-driving in a controlled set of numerical experiments. We test both methods in the Athena++ solver using (a) an analytical flux-emergence model (Y. Fan & S. Gibson 2003) and (b) a \"ground-truth\" reference simulation (S. Toriumi & S. Takasao 2017; S. Toriumi et al. 2020) of active region emergence. For E-driving, the electric field is incorporated into Athena++'s constrained-transport (CT) update, preserving the discrete solenoidal constraint. We assess the reproduction of (i) boundary magnetic flux, (ii) relative magnetic helicity, (iii) total and free magnetic energy, and (iv) magnetic morphology. Across these diagnostics, E-driving gives better overall reproduction of the reference evolution than B-driving. For the configurations considered in an Eulerian CT scheme, E-driving is more accurate than the commonly used ghost-cell B-driving strategies and simpler than constructing an update-consistent B-driving boundary condition.", "published": "2026-10-08T03:40:21Z", "updated": "2026-10-08T03:40:21Z", "authors": [ "Kyriakos Christos Tapinou", "Axel Raboonik", "David I. Pontin", "Michael S. Wheatland", "Mark C. M. Cheung", "Hannah Schunker" ], "url": "https://arxiv.org/abs/2610.11182v1", "categories": [ "astro-ph.SR", "physics.plasm-ph" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11182", "revision": 1, "status": "ready", "source_fingerprint": "adada83422f109c17e3c2b177c9d5307267652bbcd5c58e54349ec8227776d0f", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11182v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11182v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.280Z", "reason": "论文比较太阳大气磁流体模拟中的两种数据驱动边界策略，主题是太阳磁通浮现数值建模，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（实际章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We systematically quantify the performance of B- and E-driving in a controlled set of numerical experiments.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11404", "revision": 1, "title": "Oxygen isotopic ratio in open cluster RGB stars: A new method for accurate mass and age estimations", "abstract": "Determining precise and homogeneous absolute ages of open clusters (OCs) remains a challenge in stellar astrophysics, mainly due to parameter degeneracies in photometric methods and line-of-sight extinctions. We present a novel method for estimating the ages of intermediate-age and old OCs, based on the strong initial-mass dependence of the surface oxygen isotopic ratio, 16O/17O, measured in RGB stars following the first dredge-up. Using updated theoretical stellar models computed with the FuNS code, we demonstrate how post-FDU CNO isotopic abundances reflect initial stellar masses. We analysed high-resolution near-infrared spectra for 11 RGB stars belonging to four Galactic OCs. For the intermediate-age clusters NGC 7789, NGC 7044, and NGC 6819, we derive ages of 1.80, 1.81, and 2.31 Ga, respectively. For the two stars in NGC 6819 the derived initial stellar mass (1.625 Mo) and age are in excellent agreement with independent estimates from asteroseismology and eclipsing binaries. Conversely, ages estimated by means of machine learning algorithms, trained to recognise specific features in the cluster CMDs, are systematically lower. Regarding the old and super-metal-rich cluster NGC 6791, the low signal-to-noise ratio and the possible line blending hinder precise mass and age constraints. With these limitations, we can only fix a lower bound of about 4 Ga for its age. The surface oxygen isotopic ratio in RGB stars provides a powerful, independent stellar clock, making high-resolution near-infrared spectroscopy of oxygen isotopes a key tool for Galactic archaeology.", "published": "2026-10-08T07:35:16Z", "updated": "2026-10-08T07:35:16Z", "authors": [ "O. Straniero", "C. Abia", "I. Domínguez", "P. de Laverny" ], "url": "https://arxiv.org/abs/2610.11404v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11404", "revision": 1, "status": "ready", "source_fingerprint": "75a142abf8f7d828ba5ff8a5ce348b6e14b6df1b5ebeef1e37073c518926972c", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11404v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11404v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.280Z", "reason": "论文利用 RGB 星的氧同位素比估算疏散星团年龄和恒星质量，属于恒星演化与银河考古研究，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要（实际章节标题：unknown）", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The surface oxygen isotopic ratio in RGB stars provides a powerful, independent stellar clock”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11530", "revision": 1, "title": "Gaseous SiO and Silicate Clouds in Three Benchmark Early-L Dwarfs", "abstract": "Tracing silicon from gaseous SiO into silicate condensates provides a direct view of the condensation process that forms silicate clouds in L-dwarf atmospheres. Here we present evidence for gaseous SiO in three benchmark early-L dwarfs, HD 89744B, GJ 1048B, and LSPM J0632+5053B, using JWST/NIRSpec and MIRI spectroscopy. Atmospheric retrievals with and without SiO under multiple cloud prescriptions identify the strongest SiO signatures at 4.0--4.2 and 7.7--8.2 $μ$m, with the local likelihood diagnostic reaching $4.6σ$. In the physical cloud retrievals, the 8 $μ$m band probes lower pressures than the 4 $μ$m overtone, reaching atmospheric layers where equilibrium SiO is more strongly depleted by silicate condensation. All three objects also show compact Fe opacity at pressures of a few bar. Their inferred gas-phase C/O ratios are consistent with expectations from the host-star compositions after accounting for refractory oxygen sequestration. Within the adopted Mie treatment of amorphous silicate grains, the silicate mineralogies favor Mg$_2$SiO$_4$ for HD 89744B and a mixed Mg$_2$SiO$_4$+MgSiO$_3$ cloud for GJ 1048B. Extending this framework to cooler L dwarfs will trace the coupled evolution of gaseous SiO depletion and silicate-cloud formation along the L-dwarf sequence.", "published": "2026-10-08T08:58:21Z", "updated": "2026-10-08T08:58:21Z", "authors": [ "Zhijun Tu", "Shu Wang", "Xiaodian Chen", "Haomiao Huang", "Jifeng Liu" ], "url": "https://arxiv.org/abs/2610.11530v1", "categories": [ "astro-ph.SR", "astro-ph.EP" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11530", "revision": 1, "status": "ready", "source_fingerprint": "8b551cc7d949f85695b214849b2de69cd00754f243b45a10a76f7289ead4df0f", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11530v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11530v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.281Z", "reason": "论文研究早 L 型矮星大气中的气态 SiO 与硅酸盐云，与高能瞬变天体物理及所列核心方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Here we present evidence for gaseous SiO in three benchmark early-L dwarfs, HD 89744B, GJ 1048B, and LSPM J0632+5053B, using JWST/NIRSpec and MIRI spectroscopy.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11541", "revision": 1, "title": "Isotopic ratios as probes of star formation and the origin of molecular gas in the Central Molecular Zone", "abstract": "The Central Molecular Zone (CMZ) contains most of the dense molecular gas in the Milky Way but forms stars at a surprisingly low rate. Isotopic ratios provide a unique tool to investigate both the local physical conditions and the nucleosynthetic history of this gas. I summarize recent isotopic studies toward the molecular cloud G$+$0.693$-$0.027. Deuterium fractionation (D/H ratios) reveals a cold ($T_{\\rm kin}\\lesssim30$ K), relatively quiescent gas component embedded within the otherwise warm and turbulent CMZ, indicating that the earliest stages of star formation can survive in this extreme environment. I also present new $^{12}$C/$^{13}$C measurements from HC$_3$N and HC$_5$N, including the first constraints from doubly substituted $^{13}$C isotopologues. After accounting for isotopic fractionation with astrochemical models, the inferred elemental ratio ($\\sim37$--48) exceeds the canonical CMZ assumed value ($\\sim$20), supporting a scenario in which the Galactic center is replenished by less chemically processed gas flowing inward along the Galactic bar.", "published": "2026-10-08T09:10:03Z", "updated": "2026-10-08T09:10:03Z", "authors": [ "Laura Colzi" ], "url": "https://arxiv.org/abs/2610.11541v1", "categories": [ "astro-ph.GA", "astro-ph.SR" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.11541", "revision": 1, "status": "ready", "source_fingerprint": "d75512839a56e4a66ea55683345d1c9c8da542518da5f9391f96c3572495ea47", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11541v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11541v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.281Z", "reason": "论文通过同位素比研究银河系中央分子区的气体条件、恒星形成与气体来源，与所列高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The Central Molecular Zone (CMZ) contains most of the dense molecular gas in the Milky Way but forms”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11588", "revision": 1, "title": "Measuring radial flows in disc galaxies", "abstract": "Numerous theoretical studies suggest that gas accretion from the intergalactic medium is essential to feed star formation in galaxies throughout cosmic time. However, the mechanism of gas accretion remains poorly understood, as direct evidence is lacking. In some models, gas accretion is expected to take place in the outer discs of galaxies, from where it should be transferred to the inner star-forming discs through radial flows. Finding such flows and quantifying them, therefore, opens the possibility of inferring the detailed properties of the accreting gas. Unfortunately, detecting radial flows is challenging due to the large disparity between radial and rotational velocities. Additionally, the distortions in velocity fields produced by these flows resemble the effects of warped structures, further complicating their quantification. To address this, we have developed a new methodology to measure axisymmetric radial velocities in disc galaxies. Relying on the 3D kinematic fitting software \\texttt{$^{\\rm 3D}$Barolo}, we have designed a dedicated workflow to measure axisymmetric radial motions in disc galaxies and to obtain robust uncertainty estimates through a bootstrapping approach. We validated this approach using realistic axisymmetric mock galaxies as well as a small sample of `observed' Milky Way-like galaxies drawn from the TNG50 hydrodynamic simulation. These tests demonstrate that our method works well and is capable of overcoming the degeneracy between radial motions and warps. The TNG50 galaxies we analysed have large regions in their discs with non-axisymmetric inflows and outflows, but they show, on average, no global trend of coherent radial flows.", "published": "2026-10-08T09:38:39Z", "updated": "2026-10-08T09:38:39Z", "authors": [ "Yi He", "Filippo Fraternali", "Pavel E. Mancera Piña", "Enrico M. Di Teodoro" ], "url": "https://arxiv.org/abs/2610.11588v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.11588", "revision": 1, "status": "ready", "source_fingerprint": "c66852892efc431a0ccb5ef9f487cfe7385e591b790fcca5d4130db8df845aa1", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11588v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11588v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.281Z", "reason": "论文开发盘星系轴对称径向流的测量方法，主题是星系气体流动，与所列高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “To address this, we have developed a new methodology to measure axisymmetric radial velocities in disc galaxies.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11606", "revision": 1, "title": "Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D", "abstract": "We present a new radio continuum study of the Large Magellanic Cloud supernova remnant N 132D using observations from the Australia Telescope Compact Array (ATCA) and MeerKAT. The radio morphology shows a clear spatial correlation with the X-ray emission in the central and left regions of the remnant, as well as in the right portion of the shell, indicating a close connection between the thermal and non-thermal plasma components. Polarisation measurements reveal predominantly radial magnetic fields, with mean fractional polarisations of 1.2 per cent, 3.0 per cent, and 4.0 per cent at 2100, 5500, and 9000 MHz, respectively. There is also a complex structure in the Faraday Depth spectrum, showing a double-peaked profile that indicates regions with differing magnetisation properties or varying magnetic field geometry. The rotation measure derived from ATCA data has an average value of ~2 rad m^-2, with a maximum of ~338 rad m^-2. We estimate a constant partition magnetic field of ~90 microG and a minimum energy of 3 x 10^50 erg, which is in a constant partition between the energy density of electrons and the energy density of the magnetic field. The integrated radio spectrum follows a power law with a spectral index of -0.74 +- 0.01. These results provide new constraints on the magnetic field structure and energetic properties of N 132D and offer insight into particle acceleration and shock evolution in young supernova remnants.", "published": "2026-10-08T09:50:40Z", "updated": "2026-10-08T09:50:40Z", "authors": [ "Rami Z. E. Alsaberi", "Zachary J. Smeaton", "Miroslav D. Filipovic", "Roland Kothes", "Hidetoshi Sano", "Ahmed H. Abdullah", "Dejan Urovsevic", "Sanja Lazarevic" ], "url": "https://arxiv.org/abs/2610.11606v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11606", "revision": 1, "status": "ready", "source_fingerprint": "7af0d599665e4e84fe9776424ce47c443320c3ba2538da758af0c41b6d4b766a", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11606v1", "inspected_sections": [ "Introduction", "Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D", "1 Introduction", "30 Dor", "2 Observations and Analysis", "2.1 Radio Observations", "2.1.1 ATCA Observations", "2.1.2 MeerKAT Observations", "2.2 Optical Observations", "2.3 X-ray Observations", "3 Results and discussion", "3.1 Morphology", "3.2 Polarisation, Rotation Measure, and Magnetic Field Strength", "3.3 Spectral Index", "4 Conclusion", "Acknowledgments", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11606v1", "locator": "Introduction; Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D; 1 Introduction; 30 Dor; 2 Observations and Analysis; 2.1 Radio Observations; 2.1.1 ATCA Observations; 2.1.2 MeerKAT Observations; 2.2 Optical Observations; 2.3 X-ray Observations; 3 Results and discussion; 3.1 Morphology; 3.2 Polarisation, Rotation Measure, and Magnetic Field Strength; 3.3 Spectral Index; 4 Conclusion; Acknowledgments; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "c039a4fb40df2777978d7b4dec76881adea898cdffd544385092165e115e609e" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:27:22.542Z", "reason": "该工作聚焦于大麦哲伦云中龄富氧超新星遗迹 N 132D 的射电多频连续谱成像与偏振性质，研究遗迹的大尺度形态、法拉第旋转与扩散激波粒子加速能谱，与超新星早期激波破越、致密天体中心引擎、高能中微子或 FRB/PRS 等瞬变源物理无实质联系。", "result": "测得 N 132D 最大旋转测度 $RM = 338\\,{\\rm rad\\,m^{-2}}$，视线向磁场 $B_\\parallel \\sim 7.9\\,\\mu{\\rm G}$；能量均分磁场强度约 $90\\,\\mu{\\rm G}$，对应最小能量 $E_{\\rm min} = 3.3 \\times 10^{50}\\,{\\rm erg}$，显著高于激波压缩场强（$\\sim 20\\,\\mu{\\rm G}$）；空间积分射电能谱指数为 $\\langle\\alpha\\rangle = -0.74 \\pm 0.01$，整体呈现向上弯曲（concave-up）特征。", "reading_entry": "3.2 Polarisation, Rotation Measure, and Magnetic Field Strength", "problem": "大麦哲伦云最亮富氧超新星遗迹 N 132D 缺乏高精度的多频偏振与宽带射电连续谱测量，其激波磁场放大机制与电子能谱曲率尚未完全厘清。", "method": "利用 ATCA（2100、5500 与 9000 MHz）及 MeerKAT（856–1712 MHz）开展宽带射电连续谱与 Stokes $Q, U$ 偏振观测，应用法拉第旋转合成技术重建法拉第深度谱；结合旋转测度公式 $RM = 811.9 \\int_{0}^{L} n_e B_\\parallel dl$ 及能均分模型计算磁场强度。", "assumptions": [], "limits": [], "citation_leads": [ "Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D: “Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D”", "3.2 Polarisation, Rotation Measure, and Magnetic Field Strength: “$RM = 811.9 \\int_{0}^{L} n_e B_\\parallel dl$”", "3.3 Spectral Index: “$\\langle\\alpha\\rangle = -0.74 \\pm 0.01$”" ], "research_progress": "获得了 N 132D 高分辨率射电偏振图与法拉第深度谱分布，精确测定了全遗迹射电能谱指数 $\\langle\\alpha\\rangle = -0.74 \\pm 0.01$ 及其向上弯曲特征，为年轻至中龄超新星遗迹中的非线性激波粒子加速与磁场放大提供了观测证据。", "figures": [ { "url": "/arxiv-figures/2610.11606/x-ray_HST_image_final.png", "caption": "Figure 1: Images of N 132D with 2100 MHz contours overlaid (top), 5500 MHz contours overlaid (middle), and 9000 MHz contours overlaid (bottom). Left: ATCA intensity image at 2100 MHz (top), 5500 MHz (middle), and 9000 MHz (bottom). The white circles in the lower left corner represent the synthesised beams: 4 × 4 4\\times 4 arcsec 2 at 2100 MHz, and 3 × 3 3\\times 3 arcsec 2 at both 5500 and 9000 MHz. Middle: Broadband Chandra X-ray images. Right: HST [O iii ] filter images, where darker regions correspond to higher emission, while brighter regions indicate lower emission.", "label": "Fig. 1", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false }, { "url": "/arxiv-figures/2610.11606/all_regions_radial_profiles.png", "caption": "Figure 2: Normalised radial intensity profiles of the SNR derived from the optical ([O iii ]), radio (2100 MHz), and X-ray (broadband) images for the north, east, south, and west regions, extending to 90 arcsec from the adopted geometric centre (RA (J2000) = 05 h 25 m 03.1 s , Dec (J2000) = –69 ∘ 38 ′ 22.3 ′′ ).", "label": "Fig. 2", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11637", "revision": 1, "title": "Gravitational Microlensing", "abstract": "Gravitational microlensing is a unique planet-detection method that does not rely on detecting light from the host star or planet. Instead, planets are discovered when their gravitational field perturbs the light coming from a distant source. The mechanics of this method offer several advantages. It has the ability to detect wide-orbit planets of various masses around host stars of different types, at and beyond the system's snow line. Thus, microlensing complements the other detecting techniques that are more sensitive to close-orbit or high-mass planets. In this Chapter, we review the microlensing method and discuss how the physical properties, such as mass and distance, can be extracted from the microlensing light curve or from additional high-angular resolution observations. Microlensing is essential for the broader context of exoplanet demographics, as it can place constraints on planets, in wide orbits, beyond the {\\it snow line}. Studying this parameter space can help us unravel the details of planet formation and how our own Solar System formed. Lastly, we provide an example of how to model a light curve and obtain accurate physical parameters for the host and planet.", "published": "2026-10-08T10:15:55Z", "updated": "2026-10-08T10:15:55Z", "authors": [ "Aikaterini Vandorou", "Stela Ishitani Silva" ], "url": "https://arxiv.org/abs/2610.11637v1", "categories": [ "astro-ph.EP", "astro-ph.GA", "astro-ph.IM", "astro-ph.SR" ], "primary_category": "astro-ph.EP", "analysis": { "arxiv_id": "2610.11637", "revision": 1, "status": "ready", "source_fingerprint": "3ffb2dc07eaf7f33a26c44d9e6f31326e50ceecabbb4855aaf57ebd8ca890ae5", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11637v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11637v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T02:00:56.281Z", "reason": "论文讨论引力微透镜探测系外行星及行星形成，与指定的高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Gravitational microlensing is a unique planet-detection method that does not rely on detecting light from the host star or planet.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11712", "revision": 1, "title": "Nonreciprocal black holes with primary hair in beyond Horndeski gravity: Exact solutions and stability", "abstract": "We develop a novel systematic method for constructing exact, static, and asymptotically flat black-hole solutions in shift-symmetric and $Z_2$-symmetric beyond Horndeski theories. In contrast to previous studies, our approach does not rely on the restrictive reciprocal condition $g_{tt}g_{rr}=-1$, allowing for more general geometries characterized by two independent metric functions. The resulting solution space contains two qualitatively distinct types of hair originating from different branches of the theory. One branch is characterized by khronometric hair, while the other by genuine scalar hair. In both, the scalar profile defines a nontrivial preferred foliation, but the shift-symmetry Noether current and the associated propagating degree of freedom are trivial for the former and nonvanishing for the latter. Focusing mainly on the second branch, we derive several distinct families of exact black-hole solutions. In general, these solutions are singular and exhibit primary scalar hair associated with an independent scalar charge. Nevertheless, we demonstrate that they can be regularized to yield regular black-hole or solitonic configurations, for which the scalar hair becomes secondary. We further investigate the stability properties of these solutions under linear perturbations by analyzing the axial sector and the monopole $(\\ell=0)$ mode of the even-parity sector. For representative solutions with scalar hair, the perturbative analysis provides evidence for linear stability under the modes considered.", "published": "2026-10-08T11:17:39Z", "updated": "2026-10-08T11:17:39Z", "authors": [ "Sebastian Bahamonde", "Theodoros Nakas", "Simon Iteanu" ], "url": "https://arxiv.org/abs/2610.11712v1", "categories": [ "gr-qc", "astro-ph.HE", "hep-th" ], "primary_category": "gr-qc", "analysis": { "arxiv_id": "2610.11712", "revision": 1, "status": "ready", "source_fingerprint": "7dd8c991f9da7a5e670c5d62f094481f4a27f9264074c55eb49db27f52b8bc9b", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11712v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11712v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.157Z", "reason": "论文研究 beyond Horndeski 引力中的静态黑洞解及其线性稳定性，与所列瞬变天体、辐射机制或高能观测方向没有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We further investigate the stability properties of these solutions under linear perturbations”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11762", "revision": 1, "title": "Probing Massive Star Formation with Intrinsic Multiplicity Constraints from TESS Eclipsing Binaries", "abstract": "Massive stars play a central role in stellar and galactic evolution as progenitors of supernovae, neutron stars, black holes, and gravitational wave sources. Despite their importance, the dominant formation mechanisms of massive binaries remain poorly constrained observationally. We aim to use a large, homogeneous sample of eclipsing binaries to observationally constrain binary formation across a wide range of primary masses and test predictions from various formation scenarios. We combine photometric time series data from TESS with distance measurements from Gaia DR3 and near infrared photometry from 2MASS to analyze an all-sky sample of eclipsing binaries. By accounting for observational and geometric selection effects, we derive bias corrected estimates of the binary fractions and orbital parameter distributions across different mass bins. We derive bias corrected binary fractions and bias corrected distributions of orbital period and radius-to-separation ratio for systems spanning primary masses from 1.1 Msun to 47 Msun. For primary masses up to 5 Msun, the observed distributions show close agreement with theoretical predictions for systems formed via disk fragmentation followed by migration. At higher masses, we observe an apparent deficit of very short period systems relative to theoretical expectations, although this regime is also expected to be affected by incompleteness. Overall, the observed properties exhibit a gradual transition across the full range of primary masses. Within the orbital period range accessible to our sample, the results do not require a sharp transition in binary properties between F- and O-type stars. The observed continuity is consistent with disk fragmentation followed by migration acting across a broad range of stellar masses, although the present data do not uniquely require this formation pathway and alternative channels may also contribute.", "published": "2026-10-08T11:46:44Z", "updated": "2026-10-08T11:46:44Z", "authors": [ "Jasmine Vrancken", "Alex Kemp", "Andrew Tkachenko", "Conny Aerts", "Hugues Sana" ], "url": "https://arxiv.org/abs/2610.11762v1", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11762", "revision": 1, "status": "ready", "source_fingerprint": "c299969b2926743255bd668b850a2060808e9215a222f785cef679a647bb342a", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11762v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11762v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.158Z", "reason": "论文研究大质量双星的形成及其轨道参数分布，虽涉及超新星和致密星前身，但并未实质研究所列的瞬变天体物理问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The observed continuity is consistent with disk fragmentation followed by migration acting across a broad range of stellar masses”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11763", "revision": 1, "title": "Metallicity does not reorder line-to-line sensitivity to granulation in solar-like stars", "abstract": "Stellar granulation imprints line-dependent wavelength shifts and profile variations that limit the precision of radial velocity (RV) measurements used for exoplanet detection and characterization. Understanding how the sensitivity of individual spectral lines to granulation depends on stellar parameters is therefore essential for mitigating granulation-induced RV signals. Here, we investigate the effect of metallicity using MURaM 3D magnetohydrodynamic simulations of stellar granulation including a small-scale dynamo for metallicities $\\mathrm{M/H}=\\{-1.0,-0.5,0.0,0.3,0.5\\}$. We synthesize spectra of neutral and ionized lines spanning a broad range of lower excitation potentials and transition probabilities using the MPS-ATLAS code, assuming local thermodynamic equilibrium. We quantify the sensitivity to granulation using the continuum-intensity-weighted standard deviations of the line centre-of-gravity wavelength and equivalent width, denoted by $σ_λ$ and $σ_W$, respectively. Both metrics increase systematically with metallicity at disc centre owing to the combined effects of more vigorous convection and metallicity-dependent changes in the line opacity. We find that the correlation between the solar ($\\mathrm{M/H}=0.0$) and non-solar sensitivity metrics remains high from the disk center to the stellar limb. This indicates that the relative ordering of line sensitivities is robust against changes in viewing angle and metallicity. Consequently, line masks calibrated on the solar spectrum can be reliably applied to radial-velocity measurements of stars with non-solar metallicities, provided they have solar effective temperature and surface gravity.", "published": "2026-10-08T11:47:01Z", "updated": "2026-10-08T11:47:01Z", "authors": [ "Dušan Vukadinović", "Sowmya Krishnamurthy", "Valeriy Vasilyev", "Veronika Witzke", "Andrew Collier Cameron" ], "url": "https://arxiv.org/abs/2610.11763v1", "categories": [ "astro-ph.SR", "astro-ph.EP" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11763", "revision": 1, "status": "ready", "source_fingerprint": "aa046ef7045e9bce05c8c58dd9e1810e6abf7cef037694440a63145905ab1650", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11763v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11763v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.159Z", "reason": "论文关注太阳类恒星颗粒对径向速度测量的影响及系外行星观测方法，与高能瞬变天体物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “line masks calibrated on the solar spectrum can be reliably applied to radial-velocity measurements of stars with non-solar metallicities”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11799", "revision": 1, "title": "What powers the most energetic flares in the Kepler field? Revisiting the superflaring star KIC 2852961", "abstract": "Flare activity in red giants is quite common when continuously monitored with high-precision space photometry. In fact, the most powerful flares, also known as \"superflares\" have been observed on red giant stars. KIC 2852961 is a red giant star producing the highest-energy flares in the Kepler field, and is also known for its large-amplitude starspot-induced light variations. Our goal is to find out what causes the extreme flare activity and flare energies in this star. For our investigations, we use ground-based spectroscopic measurements and space photometric data, which we process using standard tools. We also collect relevant data from databases of large surveys such as Gaia. Our new radial velocity data confirm that the red giant star is part of a close binary system, in which tidal forces play a crucial role in controlling the evolution of the binary system. Our results show that tidal evolution has driven the system close to orbital circularization and rotational synchronization, but it did not completely constrain the differential rotation of the red giant, in which the magnetic dynamo can operate extremely efficiently. We find that high-energy (super)flares are primarily controlled by the internal magnetic activity of the active giant component, rather than phase-dependent interactions with the secondary star. The large spot-induced rotational light modulations indicate extensive starspots that can store enormous amounts of magnetic energy. This provides the conditions for the formation of extremely large flares, confirming the close relationship between large spot coverage and high flare energies and/or frequency. Behind all this, differential rotation may play a dual role in the flare activity of KIC 2852961: it contributes both to the formation of large starspots and to the shearing and twisting of coronal magnetic fields that can power energetic superflares.", "published": "2026-10-08T12:09:59Z", "updated": "2026-10-08T12:09:59Z", "authors": [ "Zs. Kővári", "B. Seli", "L. Kriskovics", "K. Oláh", "P. Odert", "M. Leitzinger", "B. Schmercz", "K. Vida", "R. Greimel", "B. Cseh", "A. Görgei", "T. Granzer", "P. Sági", "M. Weber" ], "url": "https://arxiv.org/abs/2610.11799v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11799", "revision": 1, "status": "ready", "source_fingerprint": "e93db9b6361f1295e73708f200c8af355ecdbb0531eca4f37d342adc59b9eb48", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11799v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11799v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.160Z", "reason": "研究对象是红巨星双星中的恒星磁活动与超级耀斑，未涉及所列高能瞬变、超新星遗迹或致密天体高能观测方向。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “high-energy (super)flares are primarily controlled by the internal magnetic activity of the active giant component”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11832", "revision": 1, "title": "Investigating the nature of magnetic turbulence in Tycho's SNR using X-ray observation", "abstract": "Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic ray acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration (DSA) mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal X-ray flux image of Tycho's SNR. This image was obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho's SNR. Additionally, we use the X-ray rim thickness measured across Tycho which is an indicator of magnetic field strength to estimate the magnetic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.", "published": "2026-10-08T12:27:34Z", "updated": "2026-10-08T12:27:34Z", "authors": [ "Ashwin Aravindaraj", "Hui Zhu", "Adrien Picquenot", "Hsiang-Kuang Chang" ], "url": "https://arxiv.org/abs/2610.11832v1", "categories": [ "astro-ph.HE" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.11832", "revision": 1, "status": "ready", "source_fingerprint": "369111b9e79d29bd43246ad651bc13709f28469788c3d6932537c2b8e514b644", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.11832v1", "inspected_sections": [ "1 Introduction", "2 Data Analysis", "2.1 Observation", "2.2 pGMCA", "2.3 Two-point correlation", "2.4 Magnetic energy spectrum using non-thermal flux image", "3 X-ray rim thickness", "3.1 Magnetic energy spectrum using X-ray rim thickness", "4 Discussion", "Appendix A" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.11832v1", "locator": "1 Introduction; 2 Data Analysis; 2.1 Observation; 2.2 pGMCA; 2.3 Two-point correlation; 2.4 Magnetic energy spectrum using non-thermal flux image; 3 X-ray rim thickness; 3.1 Magnetic energy spectrum using X-ray rim thickness; 4 Discussion; Appendix A", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "4db2d9eb7e979d98e1bd2e539d9723c2d3e642b6c721cb26ee9b22af05c8b139" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:58:14.535Z", "reason": "本文利用 Chandra X 射线观测研究成熟超新星遗迹 Tycho SNR 激波前沿的磁湍流性质及宇宙线扩散激波加速（DSA）机制，与本组关注的超新星早期激波破越、中心引擎、FRB/PRS、相对论喷流或高能中微子等瞬变物理方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "1 Introduction", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Investigating the nature of magnetic turbulence in Tycho’s SNR using X-ray observation: “Investigating the nature of magnetic turbulence in Tycho’s SNR using X-ray observation”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11855", "revision": 1, "title": "Testing Extra-Dimensional Gravitational-Wave Polarizations with Compact-Binary Observations", "abstract": "Extra spatial dimensions arise naturally in theories beyond four-dimensional general relativity (GR), but direct observational evidence remains elusive. Gravitational waves offer a distinctive probe: geometric projection onto the observable three-dimensional spatial subspace can produce apparent tensor, vector, and scalar polarizations. We consider one additional spatial dimension and a two-mode tensor-wave ansatz for which the projected polarization components are fixed linear combinations of the same two underlying GR tensor waveforms. These components enter the measured strain through the standard detector antenna patterns. A frequency-domain Bayesian analysis of five compact-binary events constrains two rotation angles for two noncommuting orderings of rotations that preserve propagation within the observed subspace. Two events are further analyzed for four orderings that allow propagation to tilt into the extra dimension. For GW250114, the maximum GR quantiles among the tested rotation orderings are $Q_{\\mathrm{GR}}\\simeq0.6\\%$ for the two-angle fits and $Q^{\\mathrm{marg}}_{\\mathrm{GR}}\\simeq4.6\\%$ for the three-angle fits after marginalizing over the third angle. Across the full event sample, the GR reference point lies inside the estimated 90% highest-posterior-density region in every case.", "published": "2026-10-08T12:38:35Z", "updated": "2026-10-08T12:38:35Z", "authors": [ "Hai-Tian Wang", "Dicong Liang", "Lijing Shao", "Yu-Xiao Liu" ], "url": "https://arxiv.org/abs/2610.11855v1", "categories": [ "gr-qc", "astro-ph.HE" ], "primary_category": "gr-qc", "analysis": { "arxiv_id": "2610.11855", "revision": 1, "status": "ready", "source_fingerprint": "94fac62d896428809ae95ee12d6d5cd23ff4b9ae8a0e68911a007db25b11aade", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11855v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11855v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.160Z", "reason": "论文检验的是紧致双星引力波信号中的额外维度与极化模式，不涉及所列高能瞬变、超新星中心引擎或致密天体高能观测，因而与本批核心研究方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “A frequency-domain Bayesian analysis of five compact-binary events constrains two rotation angles”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11983", "revision": 1, "title": "Magnetic flux cancellation in a 3D magnetohydrodynamic simulation of an emerging flux tube with a non-uniform twist", "abstract": "Flux emergence is often accompanied by flux cancellation, which may drive dynamic phenomena in the solar atmosphere. We studied magnetic flux cancellation in a three-dimensional resistive magnetohydrodynamic (MHD) simulation of an emerging flux tube with a non-uniform twist profile. We solved time-dependent resistive MHD equations to model flux emergence into a magnetised background atmosphere. We identified several cancellation sites, estimated their cancellation rates, and examined the magnetic topology and associated jet activity. The non-uniform twist produced multiple opposite photospheric polarities, leading to a complex multipolar magnetic configuration rather than a simple dipolar structure. Interactions between inner secondary magnetic patches resulted in flux cancellation of the photospheric $B_z$ along their polarity inversion line (PIL). These interactions led to the formation of concave-up loops and a cancellation rate of $1.1 \\times 10^{19}$ Mx hr$^{-1}$. During cancellation, magnetic reconnection between converging opposite polarities progressively created a coherent magnetic flux rope above the cancellation region. The evolution of the rope was associated with a blowout jet, as the rope expanded and released part of its stored twist into the overlying corona. We also examined two smaller secondary cancellation events at photospheric heights. Our results highlight the role of internal flux cancellation in restructuring the magnetic field and driving blowout-jet activity in emerging regions.", "published": "2026-10-08T13:57:00Z", "updated": "2026-10-08T13:57:00Z", "authors": [ "V. Agalianou", "S. Patsourakos", "V. Archontis" ], "url": "https://arxiv.org/abs/2610.11983v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.11983", "revision": 1, "status": "ready", "source_fingerprint": "ca315d4c4aae393a68749a5711ac5f47c99145b135e29c3e32ea57a7aab98309", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11983v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11983v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.161Z", "reason": "论文研究太阳大气中的磁通量浮现、抵消及日冕喷流，与所列高能瞬变天体物理方向没有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The evolution of the rope was associated with a blowout jet, as the rope expanded and released part of its stored twist into the overlying corona.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.11985", "revision": 1, "title": "Gas-phase chemistry of $\\mathrm{C}_3\\mathrm{H}_3^+$: a key building block for carbon mass growth in space", "abstract": "The gas-phase chemistry of $\\mathrm{C}_3\\mathrm{H}_3^+$ plays a central role in the growth of carbonaceous species across a wide range of environments, from combustion systems to interstellar media. However, the presence of multiple isomers, primarily the linear propargyl cation and the cyclic cyclopropenyl cation, has so far prevented the determination of reliable isomer-specific reaction kinetics. In this work, we combine tunable vacuum-ultraviolet (VUV) photoionization with controlled ion--molecule reaction measurements to selectively produce and probe the reactivity of $\\mathrm{C}_3\\mathrm{H}_3^+$ isomers. By employing a titration approach, we extract isomer-specific reaction rate coefficients and branching ratios for reactions of $\\mathrm{C}_3\\mathrm{H}_3^+$ with $\\mathrm{C}_2\\mathrm{H}_4$, $\\mathrm{C}_3\\mathrm{H}_4$, and $\\mathrm{C}_3\\mathrm{H}_6$. Our results demonstrate a strong contrast in reactivity: the most stable cyclic isomer is found to be essentially unreactive under the investigated conditions, whereas the linear isomer exhibits efficient and diverse chemistry leading to the formation of larger hydrocarbon ions. In particular, the formation of $\\mathrm{C}_6\\mathrm{H}_5^+$ is observed, providing an important intermediate in pathways toward aromatic species. These findings help resolve long-standing ambiguities in previously reported rate coefficients and provide new quantitative constraints for kinetic and astrochemical models. More broadly, this work highlights the importance of isomer-specific chemistry in carbon growth processes and demonstrates the effectiveness of VUV-based photoionization methods for disentangling complex reaction networks in the gas phase.", "published": "2026-10-08T13:57:17Z", "updated": "2026-10-08T13:57:17Z", "authors": [ "Corentin Rossi", "Jean-Christophe Loison", "Anne P. Rasmussen", "Roland Thissen", "Nandana Pattathadathil", "Christian Alcaraz", "Ugo Jacovella" ], "url": "https://arxiv.org/abs/2610.11985v1", "categories": [ "physics.chem-ph", "astro-ph.GA" ], "primary_category": "physics.chem-ph", "analysis": { "arxiv_id": "2610.11985", "revision": 1, "status": "ready", "source_fingerprint": "f92fa3f3a3d0f347698a6073713906963e0a9b1093bced4705033ebdd40e51f7", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.11985v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.11985v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.162Z", "reason": "论文聚焦星际介质碳氢离子的气相反应动力学与天体化学模型，不涉及所列高能瞬变、致密天体或相关观测问题。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Our results demonstrate a strong contrast in reactivity: the most stable cyclic isomer is found to be essentially unreactive under the investigated conditions, whereas the linear isomer exhibits efficient and diverse chemistry leading to the formation of larger hydrocarbon ions.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12043", "revision": 1, "title": "Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal Jets", "abstract": "Recurrent solar coronal jets originate from the same source region, providing a useful setting for studying the buildup, redistribution, and release of magnetic energy and helicity. However, how these quantities can characterize magnetic evolution and the onset conditions of the eruptions remains unclear. We perform a full three-dimensional (3D) thermodynamic magnetohydrodynamic simulation of recurrent jets driven by converging motions imposed at the bottom boundary. The simulation naturally produces two successive eruptions. The current-carrying helicity $H_J$ decreases during the first jet and gradually recovers between the two jets. In contrast, the free magnetic energy $E_{\\mathrm{free}}$ shows no clear accumulation after its first release. This difference indicates that $H_J$ provides information on magnetic evolution beyond that provided by $E_{\\mathrm{free}}$. Furthermore, the commonly used helicity ratio $H_J/H_V$ reaches different peaks near the onset of the two jets and is sensitive to the integration volume. By comparison, the locally normalized quantity $H_J/Φ_{\\mathrm{closed}}^2$ reaches similar peaks near the onset of both jets and is relatively insensitive to the choice among the tested integration volumes, where $Φ_{\\mathrm{closed}}$ is the single-polarity magnetic flux of the closed-field domain. These results reveal the local nature of the eruptions and suggest that $H_J$ normalized by the square of the closed magnetic flux may be a useful diagnostic of eruptive conditions.", "published": "2026-10-08T14:31:38Z", "updated": "2026-10-08T14:31:38Z", "authors": [ "Chang Zhou", "Jinhan Guo", "Yang Guo", "Jiajia Liu", "Zekun Lu", "Yuhang Gao" ], "url": "https://arxiv.org/abs/2610.12043v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.12043", "revision": 1, "status": "ready", "source_fingerprint": "fa2f6ce778f69fd8ba641f24b2ae441eafbb4a05355165be527dfb7bdef96cea", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12043v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12043v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.163Z", "reason": "论文研究太阳日冕喷流中的磁螺度与磁能诊断，属于太阳物理；此处的喷流并非所列方向中的相对论天体喷流，与高能瞬变研究无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “By comparison, the locally normalized quantity $H_J/Φ_{\\mathrm{closed}}^2$ reaches similar peaks near the onset of both jets and is relatively insensitive to the choice among the tested integration volumes”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12055", "revision": 1, "title": "Binding Energies of Astrophysically Relevant Molecules on CO$_2$ Clusters: Benchmarking and the Donor-Acceptor Origin of Surface-Dependent Binding", "abstract": "Carbon dioxide (CO$_2$) is among the most abundant interstellar ices and has been observed by JWST in water-rich mixtures and pure CO$_2$ environments. Astrochemical models adopt binding energies (BEs) measured on water ice because few BEs are available for CO$_2$ ice. We calculate BE distributions for twelve adsorbates (N$_2$, CH$_4$, HCl, C$_2$H$_2$, H$_2$S, HF, HCN, H$_2$CO, HCOOH, HNC, CH$_3$OH, H$_2$O) on CO$_2$ clusters containing two to five molecules using DFT calibrated against CCSD(T)/CBS, a coupled-cluster treatment extrapolated to the complete-basis-set limit. Binding strength depends on whether the adsorbate requires the surface to donate a hydrogen bond (H-bond). CO$_2$ can accept an H-bond but cannot donate one, and all six species compared with water ice from Ahmad et al. (2026) bind more weakly on CO$_2$. The ratio of the BE on CO$_2$ to water ice ranges from 0.66 for H$_2$CO and 0.75 for H$_2$O to 0.87 for CH$_3$OH, 0.89 for HCOOH and 0.92 for C$_2$H$_2$. Formaldehyde is predicted to desorb near 57 K from CO$_2$-rich ice, compared with 85 K from water-rich ice, and could contribute to cold gas-phase H$_2$CO. Although the mean binding energies are changing with cluster size for several species, the differences can be traced to local binding interactions likely to remain important in larger ice models. The BEs vary by more than 500 K between sites, while the desorption peaks range from 11 K for CH$_4$ to 132 K for HCOOH. The limited H-bonding capacity of CO$_2$ may favour separation of mixed H$_2$O:CO$_2$ ice into CO$_2$-rich domains.", "published": "2026-10-08T14:38:32Z", "updated": "2026-10-08T14:38:32Z", "authors": [ "Aneesa Ahmad", "Catherine Walsh", "Stefan Vogt-Geisse" ], "url": "https://arxiv.org/abs/2610.12055v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12055", "revision": 1, "status": "ready", "source_fingerprint": "2d34adf2c82a2ac40ce5f82de62d92443be2124e1d9e55feb62cea82e73da0a5", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12055v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12055v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.163Z", "reason": "论文聚焦 CO$_2$ 冰团簇表面分子吸附结合能与脱附行为，属于星际化学和冰面化学研究，与 FRB、超新星中心引擎、激波相互作用或致密天体高能观测无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Carbon dioxide (CO$_2$) is among the most abundant interstellar ices and has been observed by JWST i”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12117", "revision": 1, "title": "EWOCS-XI: Anisotropic expansion and shear in the cluster Westerlund 1. A 2D kinematic analysis with Gaia DR3", "abstract": "Westerlund 1 (Wd1) is one of the Milky Way's most massive young clusters, in which heavy extinction and field contamination have historically hampered its kinematic characterization. We aim to assess Wd1's internal kinematics, dynamical state, and formation scenario. Using a robust 5D clustering approach, we identified 559 bona fide members. We modeled their proper motions via a 2D first-order Taylor expansion to derive the velocity gradient tensor, mapping expansion, rotation, and shear. Restricting the kinematic analysis to 524 stars with proper motion uncertainties $<0.5~\\mathrm{mas\\,yr^{-1}}$, we find at least 103 gravitationally unbound members, including 14 walkaway stars. The 2D analysis reveals a statistically significant divergence (>4$σ$) highlighting preferred expansion along the Galactic latitude (position angle $164^\\circ\\pm10.1^\\circ$). A detected cross-gradient ($\\partial v_b / \\partial l = -0.41 \\pm 0.08$ km s$^{-1}$ pc$^{-1}$) provides a clear signature of shear on the plane of the sky. Wd1 does not behave as a single cohesive population, but comprises two decoupled subsystems: a stable, bound core in dynamical equilibrium and an escaping, unbound envelope. This prominent anisotropic expansion perpendicular to the Galactic plane has a kinematic timescale ($Δt_{\\mathrm{kin}} = 2.08 \\pm 0.44$ Myr) matching the independent orbital mid-plane crossing time ($Δt_{\\mathrm{orbit}} = 2.10 \\pm 0.05$ Myr). This temporal alignment indicates the expansion onset coincided with Wd1's Galactic disk passage, triggered either by internal dynamics (e.g., early supernova feedback) or external tidal perturbations. Finally, the robust unbound population demonstrates that active cluster dissolution is underway, driven by discrete dynamical ejection events rather than long-term stellar evaporation.", "published": "2026-10-08T15:12:40Z", "updated": "2026-10-08T15:12:40Z", "authors": [ "L. Prisinzano", "F. Damiani", "C. Ordenes-Huanca", "M. Tarantino", "S. Sciortino", "N. J. Wright", "V. Almendros-Abad", "M. Andersen", "A. Bayo", "R. Bonito", "V. Cusimano", "M. Haberle", "K. Mužic", "I. Negueruela", "E. Sabbi", "A. Winter", "M. G. Guarcello" ], "url": "https://arxiv.org/abs/2610.12117v1", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.12117", "revision": 1, "status": "ready", "source_fingerprint": "027a5e65de496bbab4b8d5e57619e81710dc21d02ad3a0631d4a02f36391b516", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12117v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12117v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.164Z", "reason": "论文主要研究 Westerlund 1 星团的 Gaia DR3 五维运动学、膨胀和剪切，虽提及早期超新星反馈可能影响星团，但并未实质研究超新星中心引擎、爆发辐射、激波或致密天体高能观测。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “The 2D analysis reveals a statistically significant divergence (>4$σ$)”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12121", "revision": 1, "title": "Too many or too bright? Status and perspectives in the study of the UV Luminosity Function at z>10", "abstract": "The finding that galaxies in the first 500Myr were much more numerous and/or brighter than expected is often cited as one of the main discoveries of the James Webb Space Telescope in its first four years of operation. This result is now solidly based on an impressive number of surveys that have detected, spectroscopically confirmed, and characterized a relatively large sample of galaxies up to z=14.44, the redshift of the most distant galaxy currently known. This finding has motivated the introduction of additional physical mechanisms into theoretical models to reproduce the observed numbers and luminosities. These results contrast with the failure, despite ongoing efforts, to confirm any galaxy candidate beyond this redshift. This review summarizes the status of the search for and characterization of galaxies at z>9, focusing on the evolution of the UV Luminosity Function (UVLF), which is the main statistical description of the galaxy population that can be obtained at these redshifts. We first provide a comprehensive overview of the full set of JWST data obtained so far. We perform a 'meta--analysis' on the entire data set and provide a simple yet effective description of the global evolution of the UVLF, averaging over the various surveys. We also compare these results extensively with theoretical models that were developed to match the new JWST observations and that explore different physical mechanisms able to drive the observed evolution. We conclude with a summary of the contrasting results regarding the search for galaxy candidates at z>15, and outline the requirements for future surveys aimed at breaking this barrier.", "published": "2026-10-08T15:16:32Z", "updated": "2026-10-08T15:16:32Z", "authors": [ "A. Fontana", "H. Atek", "V. Bromm", "A. J. Bunker", "M. Castellano", "P. Dayal", "F. D'Eugenio", "D. Elbaz", "A. Ferrara", "S. L. Finkelstein", "S. Fujimoto", "M. Giavalisco", "Y. Harikane", "C. Kobayashi", "F. Pacucci", "P. G. Pérez-González", "P. Rosati", "A. Trinca", "R. Tripodi", "P. Santini", "E. Vanzella", "A. Venditti", "A. Weibel" ], "url": "https://arxiv.org/abs/2610.12121v1", "categories": [ "astro-ph.GA", "astro-ph.CO" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12121", "revision": 1, "status": "ready", "source_fingerprint": "1dc7e286d70aa362fbc81e4e682ddc9fc13e6598d0f6365b84a16b0410dca0f4", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12121v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12121v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.164Z", "reason": "论文综述高红移星系的 UV 光度函数、JWST 星系计数及早期星系形成模型，主题属于星系宇宙学，与指定的高能瞬变天体物理核心方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “This review summarizes the status of the search for and characterization of galaxies at z>9”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12143", "revision": 1, "title": "Discovery of the Slowest Radio Pulsar in the Small Magellanic Cloud", "abstract": "We report the discovery of a new radio pulsar PSR J0103$-$72 in the Small Magellanic Cloud (SMC) through a reanalysis of Parkes/Murriyang archival observations targeting supernova remnants and pulsar-wind nebulae in the SMC. Previously two pulsars were discovered in these observations, and PSR J0103$-$72 is the third which we independently detected in two observations of its target field. It has a spin period of 1.327 sec and a dispersion measure (DM) of $272\\pm13~\\mathrm{pc\\,cm^{-3}}$, making it the slowest known radio pulsar in the SMC with the second-highest DM. We did not identify any plausible supernova remnant or pulsar-wind nebula associated with the pulsar. Subtracting the predicted Galactic foreground leaves a DM contribution of $\\sim 230$--$242~\\mathrm{pc\\,cm^{-3}}$, which may suggest a long path through the ionized medium of the SMC, enhanced ionized gas along the sightline, or both. Although these data had previously been searched using both FFT and fast folding algorithms, our FFT-based reprocessing found PSR J0103$-$72 through search techniques which have previously been highly effective in discovering a large number of pulsars in other surveys. This discovery shows that candidates with weak Fourier-domain significance can reveal faint, narrow-duty cycle pulsars missed in earlier extragalactic pulsar searches.", "published": "2026-10-08T15:29:03Z", "updated": "2026-10-08T15:29:03Z", "authors": [ "Weiyu Wang", "Rahul Sengar" ], "url": "https://arxiv.org/abs/2610.12143v1", "categories": [ "astro-ph.HE", "astro-ph.GA" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12143", "revision": 1, "status": "ready", "source_fingerprint": "735746fd400cbb1549c87e1b42aab8bed85c544d3a8fab67a5433cf5ab2c010e", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12143v1", "inspected_sections": [ "Introduction", "Discovery of the Slowest Radio Pulsar in the Small Magellanic Cloud", "I Introduction", "II Observations", "III Data reprocessing", "III.1 Preprocessing", "III.2 Periodicity search", "III.3 Candidate sifting", "III.4 Folding and inspection", "III.5 Sensitivity", "IV Results", "IV.1 New discovery", "IV.2 Detection of known pulsars", "V Discussion", "V.1 The previous non-detection of PSR J0103$-$72", "V.2 Lack of association", "VI Conclusion" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12143v1", "locator": "Introduction; Discovery of the Slowest Radio Pulsar in the Small Magellanic Cloud; I Introduction; II Observations; III Data reprocessing; III.1 Preprocessing; III.2 Periodicity search; III.3 Candidate sifting; III.4 Folding and inspection; III.5 Sensitivity; IV Results; IV.1 New discovery; IV.2 Detection of known pulsars; V Discussion; V.1 The previous non-detection of PSR J0103$-$72; V.2 Lack of association; VI Conclusion", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "cd5e5fe1e8e49bf09c4e5385feeef565d9624ff4d4b725192005ae2b457ae3be" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:59:27.306Z", "reason": "本工作报道在小麦哲伦云（SMC）射电巡天归档数据中重处理发现自转周期为 1.327 s 的慢射电脉冲星 PSR J0103$-$72，并明确指出该源与超新星遗迹缺乏关联（Lack of association），属于常规河外孤立射电脉冲星搜寻，与本组核心关注的 FRB/PRS 及其周围环境、超新星中心引擎、激波破越、相对论喷流等高能瞬变物理机制无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "IV.1 New discovery", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "V.2 Lack of association: “Lack of association”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12159", "revision": 1, "title": "Modeling CO Line Luminosity Using FIRE Simulations: I. Methodology and Validation of Molecular Gas and CO Abundance", "abstract": "We present a post-processing pipeline that predicts CO line luminosities, molecular hydrogen masses, and CO abundances for galaxies in the Feedback in Realistic Environments (FIRE-2) simulations, as a first step toward CO response functions for line intensity mapping mocks. SKIRT gives the radiation field reaching each gas cell. CLOUDY, tabulated on a five-parameter grid (metallicity, density, turbulent velocity, radiation field, cloud scale) and interpolated, gives $L'_{\\rm CO(1-0)}$ and the $\\rm H_2$ and CO masses. In this first of three papers we validate the pipeline against observations. For Milky Way (MW) molecular clouds, the predicted $L'_{\\rm CO(1-0)}$ rises sharply at $A_V\\sim1$ and matches the observed values above that column. For a uniform $3\\,Z_\\odot$ the summed luminosity is within 35\\% of the observed total. A factor of three increase in metallicity changes the total $L'_{\\rm CO(1-0)}$ by an order of magnitude. Along MW sight lines, the predicted $N_{\\rm CO}/N_{\\rm H_2}$ reproduces the observed upturn within 0.3 dex in $N_{\\rm H_2}$ but falls below the data at higher columns. At $z=0$ our molecular gas masses agree with xCOLD GASS for ${\\rm SFR}\\gtrsim0.3\\,M_\\odot\\,yr^{-1}$ and are converged across our simulation resolutions. At $z\\gtrsim1$ observed gas masses exceed ours at fixed stellar mass, though selection effects and conversion-factor assumptions limit this comparison. CO luminosities are compared with extragalactic observations in Paper II. Capturing the metallicity-dependent dust shielding of CO from photodissociation is essential for modeling CO emission in low-mass and high-redshift galaxies.", "published": "2026-10-08T15:38:27Z", "updated": "2026-10-08T15:38:27Z", "authors": [ "Doğa Tolgay", "Norman W. Murray", "Dongwoo Chung", "J. Richard Bond", "Nathan J. Carlson", "Robert Feldmann", "Andrew Wetzel", "Guochao Sun" ], "url": "https://arxiv.org/abs/2610.12159v1", "categories": [ "astro-ph.GA", "astro-ph.CO" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12159", "revision": 1, "status": "ready", "source_fingerprint": "603d0f729a5d380017cb5f06c209e993af6508ada080a56f2f4b3b680d1c730e", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12159v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12159v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.165Z", "reason": "该论文聚焦星系CO谱线、分子气体和CO丰度的模拟后处理与线强度映射，不涉及FRB、超新星中心引擎、激波破越、相对论喷流、中微子或致密天体高能观测。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “Capturing the metallicity-dependent dust shielding of CO from photodissociation is essential for modeling CO emission in low-mass and high-redshift galaxies.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12199", "revision": 1, "title": "Autocorrelation in black hole flare movies: Departures from Kerr", "abstract": "Autocorrelation in black hole movies encodes the time delays and angular separations between gravitationally lensed images, offering a means of testing the spacetime geometry. Using an orbiting hot spot in the parametrized Johannsen-Psaltis metric with a single deformation parameter, we investigate the ability of lensing-induced correlations to distinguish departures from Kerr. From ray-traced movies, we extract the slope (k) and intercept (b) of an approximately linear secondary ridge in the time-angle autocorrelation map as potential future observables. Variations in the spin and the metric deformation parameter produce distinctive trajectories in the (k,b) plane, allowing the two observables to jointly constrain both parameters when the orbital radius, observer inclination, and orbital angular velocity are specified. By varying the orbital angular velocity, we construct a Kerr reference region in the (k,b) plane, and we find that, for some low-spin configurations with negative deformation parameters, the measured slope-intercept pairs of the secondary peaks lie outside this reference region. This feature appears for sub-Keplerian, Keplerian, and super-Keplerian motion, indicating that secondary-ridge measurements from black hole flare movies have the potential to distinguish non-Kerr signatures.", "published": "2026-10-08T15:53:16Z", "updated": "2026-10-08T15:53:16Z", "authors": [ "Fang-Stars Wei", "Zelin Zhang", "Zhenyu Zhang", "Bin Chen" ], "url": "https://arxiv.org/abs/2610.12199v1", "categories": [ "astro-ph.HE", "gr-qc" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12199", "revision": 1, "status": "ready", "source_fingerprint": "bf6ec610200e3a4ffb191b0689900fd8ffd2af3074940c478a549a9a48acf532", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12199v1", "inspected_sections": [ "Introduction", "Autocorrelation in black hole flare movies: Departures from Kerr", "I Introduction", "II Setup and numerical method", "II.1 Autocorrelation of black hole movies", "II.2 Johannsen-Psaltis spacetime", "II.3 Orbiting hot spot and dynamic imaging", "III Secondary ridge and measured observables", "III.1 One-parameter response in the slope-intercept plane", "III.2 Non-Kerr signatures and beyond Keplerian motion", "IV Summary and discussion", "acknowledgements", "References", "Appendix A Hot-spot emission and radiative transfer", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12199v1", "locator": "Introduction; Autocorrelation in black hole flare movies: Departures from Kerr; I Introduction; II Setup and numerical method; II.1 Autocorrelation of black hole movies; II.2 Johannsen-Psaltis spacetime; II.3 Orbiting hot spot and dynamic imaging; III Secondary ridge and measured observables; III.1 One-parameter response in the slope-intercept plane; III.2 Non-Kerr signatures and beyond Keplerian motion; IV Summary and discussion; acknowledgements; References; Appendix A Hot-spot emission and radiative transfer; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "25160b21dda40f8a2f7cb1a500abb1536bb975a9c44d330548078374aaebd4fa" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:36:51.644Z", "reason": "本工作研究利用黑洞耀发动态成像的二维时空自相关函数检验时空度规对 Kerr 度规的偏离（基于 Johannsen-Psaltis 度规及热斑轨道模型），属于黑洞强引力场几何检验与 VLBI 成像方法学研究，与本组关注的高能瞬变物理（FRB/PRS、超新星中心引擎、激波破越与周星相互作用、相对论喷流及高能中微子）无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "IV Summary and discussion", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Autocorrelation in black hole flare movies: Departures from Kerr: “Autocorrelation in black hole flare movies: Departures from Kerr”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12205", "revision": 1, "title": "Evidence for orbital eccentricity supports a hierarchical origin for GW231123", "abstract": "GW231123 is the most massive binary black hole merger observed to date and one of the most intriguing hierarchical merger candidates in the pair-instability mass gap. Its exceptionally large inferred component spins and remarkably short in-band duration make the source highly sensitive to waveform physics near merger. Here we show that GW231123 is better described as an eccentric binary black-hole merger. We analyse data over 11--448 Hz using the eccentric, spin-precessing effective-one-body waveform model TEOBResumS--Dalí, accounting for detector calibration uncertainty. We measure $e_{5.5\\,\\mathrm{Hz}}=0.34^{+0.12}_{-0.23}$ at 90\\% credibility and obtain a Bayes factor of 10.2 in favour of the eccentric model over its quasi-circular counterpart. GW231123-like injection--recovery studies further show that analyses starting at 20 Hz, as in previous studies, can obscure this eccentricity. Including eccentricity substantially changes the spin inference, weakening the preference for a near-extremal secondary spin and lowering its posterior median to $a_2\\simeq0.7$, close to the characteristic spin expected for a black-hole merger remnant. These results provide a coherent dynamical interpretation of GW231123, in which residual eccentricity, a mass-gap black hole, and a remnant-like spin arise naturally from a hierarchical merger channel in a dense environment.", "published": "2026-10-08T15:56:53Z", "updated": "2026-10-08T15:56:53Z", "authors": [ "Baoxiang Wang", "Tao Yang", "Zhoujian Cao", "Bin Hu", "Xikai Shan", "Rong-Gen Cai" ], "url": "https://arxiv.org/abs/2610.12205v1", "categories": [ "astro-ph.HE", "gr-qc" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12205", "revision": 1, "status": "ready", "source_fingerprint": "981072824927d56a15aa45dd08749f3f0f981739e8206cfb1fe73fb7be79b67b", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12205v1", "inspected_sections": [ "Introduction", "Evidence for orbital eccentricity supports a hierarchical origin for GW231123", "Results", "Evidence for orbital eccentricity", "Eccentricity inference at 10 Hz from the 20–448 Hz band", "Injection–recovery consistency analysis", "Eccentricity brings the secondary spin closer to the merger-remnant scale", "Broader source parameter consistency", "Discussion", "Methods", "Detector data and analysis band", "Waveform hypotheses", "Bayesian inference", "Calibration uncertainty", "Point-mass microlensing extension", "Acknowledgements", "Author contributions", "Competing interests", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12205v1", "locator": "Introduction; Evidence for orbital eccentricity supports a hierarchical origin for GW231123; Results; Evidence for orbital eccentricity; Eccentricity inference at 10 Hz from the 20–448 Hz band; Injection–recovery consistency analysis; Eccentricity brings the secondary spin closer to the merger-remnant scale; Broader source parameter consistency; Discussion; Methods; Detector data and analysis band; Waveform hypotheses; Bayesian inference; Calibration uncertainty; Point-mass microlensing extension; Acknowledgements; Author contributions; Competing interests; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "087eace14816b4466e902b7dab13442bbdfff81cbe957845c79bfa0bbce234ec" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:37:23.412Z", "reason": "该工作聚焦于双黑洞引力波事件 GW231123 的轨道偏心率参数估计与动力学等级并合起源（hierarchical origin），属于双黑洞引力波波形与动力学演化研究，与本组关注的 FRB/PRS、超新星中心引擎、激波破越与周星相互作用、相对论喷流及高能瞬变天体电磁/中微子观测等核心方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "Evidence for orbital eccentricity supports a hierarchical origin for GW231123", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Evidence for orbital eccentricity supports a hierarchical origin for GW231123: “Evidence for orbital eccentricity supports a hierarchical origin for GW231123”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12322", "revision": 1, "title": "JWST CAPERS: Spectroscopic evaluation of very high redshift galaxy candidates", "abstract": "JWST/NIRCam imaging has enabled efficient selection of a large number of galaxy candidates at very high redshifts. Accurate and robust selection is crucial for statistical analyses, such as measurement of the ultraviolet luminosity function (UV LF). A variety of selection methods and criteria have been proposed in the literature. We evaluate the selection methodology of galaxy candidates at $z\\geq8.5$ using 183 candidates with secure spectroscopic redshifts obtained from the CAPERS JWST/NIRSpec PRISM program. The success of high-$z$ confirmation is strongly correlated with the photometric signal-to-noise ratio (SNR) in the detection filter, the strength of the Lyman-$α$ break, and the $Δχ^2$ between the best-fitting low-redshift and high-redshift spectral energy distribution model. However, the most efficient selection method is the use of a UV LF prior on the inferred $p(z)$ of a source, raising the success rate from $\\simeq 35\\%$ to $\\simeq 77\\%$ while achieving greater completeness than conservative SNR and $Δχ^2$ cuts. Out of the 183 candidates we spectroscopically confirm 48 sources at $z\\geq8.5$ via detections of emission lines and/or the Lyman-$α$ break (particularly important for those with no emission line detection). We report the highest-redshift source in CAPERS as UDS-111893 at $z_{\\mathrm{spec}}=12.98$, with no sources confirmed at $z>13$. This work provides spectroscopic quantification of JWST/NIRCam photometric selection at $z\\geq8.5$, and demonstrates the effectiveness of a UV LF prior for high-redshift photometric selection.", "published": "2026-10-08T17:03:56Z", "updated": "2026-10-08T17:03:56Z", "authors": [ "Callum T. Donnan", "Mark Dickinson", "Lorenzo Napolitano", "Pablo Arrabal Haro", "Anthony J. Taylor", "Hollis B. Akins", "Ryan Begley", "Davide Bevacqua", "Adam C. Carnall", "Marco Castellano", "Fergus Cullen", "James S. Dunlop", "Steven L. Finkelstein", "Carter Flayhart", "Mauro Giavalisco", "Michaela Hirschmann", "Ray A. Lucas", "Derek J. McLeod", "Ross J. McLure", "Casey Papovich", "Laura Pentericci", "Borja Pérez-Díaz", "Thomas M. Stanton", "L. Y. Aaron Yung" ], "url": "https://arxiv.org/abs/2610.12322v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12322", "revision": 1, "status": "ready", "source_fingerprint": "73b8e0280105442b3e3eb4d62ce30fa5ce0666c263133ecff92f40e8f12961d6", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12322v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12322v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.166Z", "reason": "该论文聚焦 JWST 对超高红移星系候选体的光谱确认与紫外光度函数先验选择，与 FRB、超新星中心引擎、激波破越、相对论喷流或致密天体高能观测等方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “This work provides spectroscopic quantification of JWST/NIRCam photometric selection at $z\\geq8.5$”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12323", "revision": 1, "title": "Rotation period of the O giant xi Persei: Coexistence of cyclic and periodic variability. A weakly magnetic candidate star", "abstract": "OB stars exhibit line profile variability, often associated with rotation; notably, in their UV wind-sensitive lines where discrete absorption components tend to recur cyclically. We searched for periodicity in spectral regions of the O7.5III(n)((f)) star xi Persei formed very close to the star. The NIV 1718 A line was identified as the most uncontaminated spectral with a large and homogeneous available dataset is available: 307 IUE spectra over 12 years and 11 STIS spectra taken 21 years later. We also studied 322 time-resolved HeII 4686 A spectra and MOST, BRITE, and TESS space photometry, covering a time span of 13 years. We also reconsidered X-ray studies with Chandra. A CLEAN analysis and subsequent weighted least-squares fit of the flux in this region resulted in a unique period of 2.040514(20) d, attributed to rotation. The phase of maximum flux in the NIV, SiIV, Ha, and HeII line profiles coincide with the results of X-ray variability studies. This period was also found in the photometric data. Given the coherent periodic behaviour probing the region of the wind nearest the stellar surface, we propose that xi Per has an as-yet undetected weak global surface magnetic field. The sinusoidal behaviour suggested that only one magnetic pole is visible, implying an inclination of i approximately 51 deg, and therefore, 39 deg for the magnetic obliquity. We present a conceptual framework within which weak wind confinement by a global magnetic field can create a small magnetospheric disc, while allowing for the formation of more classic corotating interaction regions at higher magnetic latitudes. The periodic variations are then understood to result from the changing projected area of the magnetospheric disc as a function of rotational phase, both along the line of sight and off the stellar limb.", "published": "2026-10-08T17:05:25Z", "updated": "2026-10-08T17:05:25Z", "authors": [ "H. F. Henrichs", "N. P. Sudnik", "A. David-Uraz" ], "url": "https://arxiv.org/abs/2610.12323v1", "categories": [ "astro-ph.SR" ], "primary_category": "astro-ph.SR", "analysis": { "arxiv_id": "2610.12323", "revision": 1, "status": "ready", "source_fingerprint": "c0757715fe81eeebb8eecb3ab7d8a0559d52a74348c20c7b774b88a9c46c78c3", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12323v1", "inspected_sections": [ "Introduction", "Rotation period of the O giant $xi$ Persei: Coexistence of cyclic and periodic variability", "1 Introduction", "2 Stellar parameters", "3 Observational data", "3.1 UV spectra", "3.1.1 IUE", "3.1.2 STIS", "3.2 Optical spectroscopy: He II $lambda$4686 Å", "4 Period analysis", "4.1 UV data", "4.2 He II $lambda$4686 Å", "4.3 Revisited H$alpha$ - Chandra co-variability", "5 Interpretation of the period", "6 Space photometry", "6.1 MOST", "6.2 BRITE", "6.3 TESS", "6.4 Summary of phases", "7 Magnetic measurements", "8 Discussion", "8.1 Simultaneous UV and H$alpha$ spectroscopy", "8.2 Simultaneous X-ray observations and H$alpha$ and UV spectroscopy", "8.3 Wind magnetic confinement", "8.4 On the origin of ultraviolet line profile variability in $xi$ Per", "8.5 Investigating the origin of optical light variations", "8.6 Stochastic versus dipolar magnetic fields", "8.7 Period search in other O stars", "9 Conclusions", "Data availability", "References", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12323v1", "locator": "Introduction; Rotation period of the O giant $xi$ Persei: Coexistence of cyclic and periodic variability; 1 Introduction; 2 Stellar parameters; 3 Observational data; 3.1 UV spectra; 3.1.1 IUE; 3.1.2 STIS; 3.2 Optical spectroscopy: He II $lambda$4686 Å; 4 Period analysis; 4.1 UV data; 4.2 He II $lambda$4686 Å; 4.3 Revisited H$alpha$ - Chandra co-variability; 5 Interpretation of the period; 6 Space photometry; 6.1 MOST; 6.2 BRITE; 6.3 TESS; 6.4 Summary of phases; 7 Magnetic measurements; 8 Discussion; 8.1 Simultaneous UV and H$alpha$ spectroscopy; 8.2 Simultaneous X-ray observations and H$alpha$ and UV spectroscopy; 8.3 Wind magnetic confinement; 8.4 On the origin of ultraviolet line profile variability in $xi$ Per; 8.5 Investigating the origin of optical light variations; 8.6 Stochastic versus dipolar magnetic fields; 8.7 Period search in other O stars; 9 Conclusions; Data availability; References; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "627b23499ca1a065272020af5e437316a1dc0ddf67796058b42a44778f9ecf84" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T12:25:50.574Z", "reason": "本文聚焦于单颗孤立银河系大质量逃逸星（O 型巨星 xi Persei）的多波段光谱（UV/光学/X射线）及空间测光周期性分析，探讨其弱磁层与共转相互作用区（CIR），不涉及 FRB/PRS、超新星中心引擎、激波破越、相对论喷流或高能瞬变天体致密物理过程。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "1 Introduction", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查正文中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Rotation period of the O giant $xi$ Persei: Coexistence of cyclic and periodic variability: “A CLEAN analysis and subsequent weighted least-squares fit of the\nflux in this region\nresulted in a unique period of $2.040514\\pm 0.000020\\,$d, attributed to rotation.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [ { "url": "/arxiv-figures/2610.12323/plotBRITEred0.png", "caption": "Figure 14: Top : Folded light curve of the BRITE 2014/15 data with the rotation period. Phase 0 corresponds to BJD = 2456982.842 ± \\pm 0.027 (Eq. 5 ). The best cosine fit is overplotted in brown. Bottom : Fit residuals in the same units as the top panel. The large scatter is considered to be intrinsic.", "label": "Fig. 14", "category": "observational", "category_badge": "观测总体曲线/能谱", "is_schematic": false }, { "url": "/arxiv-figures/2610.12323/HeIIphase_c2.png", "caption": "Figure 10: Top : Phase-folded relative flux measurements of the He II λ \\lambda 4686 Å line in the interval [ − - 400, − - 225] km s -1 over 5.5 d. The best weighted cosine fit with a fixed period of 2.040514 d is overplotted. Phase 0 corresponds to HJD = 2451387.302 ± 0.022 =2451387.302\\pm 0.022 . Bottom : Fit residuals.", "label": "Fig. 10", "category": "fitting", "category_badge": "数据拟合与模型对比", "is_schematic": false } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12394", "revision": 1, "title": "Inflow-driven galaxy evolution - II: A hierarchy in the scaling relations of star-forming galaxies", "abstract": "The star-forming main sequence (SFMS; $M_\\star$--sSFR), the gas-to-stellar mass relation ($M_\\star$--$M_{\\rm gas}/M_\\star$), and the mass--metallicity relation (MZR; $M_\\star$--$Z_{\\rm gas}$) are three core scaling relations for star-forming galaxies, and together they encode the information about the baryon cycle that operates during galaxy evolution. We investigate how these relations emerge by modelling the gas flows that regulate the baryon cycle, using both an ideal and a cosmological gas flow model, and identify a hierarchy among the three relations, with one further parameter entering the scatter budget at each step. In our model, the SFMS and its scatter are set primarily by the formation time of the host halo, with a weak dependence on the star formation efficiency and the mass-loading factor. The gas-to-stellar mass relation follows from the ratio of the sSFR to the star formation efficiency, and inherits the scatter of both. The MZR in turn follows from the gas-to-stellar mass relation together with the mass-loading factor, their relative contributions depending on the galaxy evolutionary state between the inflow-driven regime and equilibrium. This hierarchy naturally introduces further correlations among the three relations, such as the fundamental plane of star formation ($M_\\star$--$M_{\\rm gas}$--SFR), the fundamental metallicity relation ($M_\\star$--SFR--$Z_{\\rm gas}$) and its gaseous counterpart ($M_\\star$--$M_{\\rm gas}$--$Z_{\\rm gas}$), and the correlations of each relation with galaxy size, which traces the star formation efficiency through the star formation law. Together, the three core scaling relations and the higher-dimensional correlations among them follow from a single framework, providing a foundation for linking the observables of star-forming galaxies to the underlying baryon cycle.", "published": "2026-10-08T17:39:50Z", "updated": "2026-10-08T17:39:50Z", "authors": [ "Kai Wang", "Carlton Baugh", "Sownak Bose", "Shaun Cole", "Carlos S. Frenk", "Cedric Lacey", "Julio F. Navarro", "Kyle A. Oman", "Amélie Saintonge", "Tom Theuns" ], "url": "https://arxiv.org/abs/2610.12394v1", "categories": [ "astro-ph.GA" ], "primary_category": "astro-ph.GA", "analysis": { "arxiv_id": "2610.12394", "revision": 1, "status": "ready", "source_fingerprint": "9e6584e88d1070dc91237dceea3914bab297c7591cb435f70b6005422d487ee1", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12394v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12394v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.166Z", "reason": "论文研究的是恒星形成星系的气体流入、质量—金属丰度等尺度关系，与指定的高能瞬变、致密天体及其辐射环境方向无实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We investigate how these relations emerge by modelling the gas flows that regulate the baryon cycle”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12429", "revision": 1, "title": "Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114", "abstract": "Testing the horizon properties of astrophysical black holes is a central goal of gravitational-wave astronomy. The recently identified Direct Wave (DW), a prompt non-quasinormal component of GW250114, provides a new probe of near-horizon physics. While it remains unclear whether the DW itself carries horizon information, we show that it enables a novel null test of horizon reflectivity. If the remnant is an exotic compact object (ECO) with a partially reflecting surface, inward plunge radiation is reflected and leaks back through the gravitational potential barrier, producing a delayed DW echo whose amplitude is set by the surface reflectivity ($|\\mathcal{R}_s|$). We construct the corresponding echo template, normalized by the observed DW, and search for it in quasinormal-mode-filtered data. We find no evidence for an echo ($\\ln\\mathcal{B}=-2.9$) and obtain the 90\\% credible bound $|\\mathcal{R}_s|<0.06$, corresponding to a reflected energy fraction below $0.4\\%$, for surfaces from $0.1\\, M_f$ to a Planck length from the would-be horizon. Our method thus turns the prompt ringdown signal into a direct test of horizon reflectivity.", "published": "2026-10-08T17:56:25Z", "updated": "2026-10-08T17:56:25Z", "authors": [ "R. Prasad", "Subhodeep Sarkar", "Sudipta Sarkar" ], "url": "https://arxiv.org/abs/2610.12429v1", "categories": [ "gr-qc", "astro-ph.HE" ], "primary_category": "gr-qc", "analysis": { "arxiv_id": "2610.12429", "revision": 1, "status": "ready", "source_fingerprint": "ab8f82e768acf1ec76ed81e8520cdeac8e68ea2ca9da4e2f74e0e75d4cd7663e", "priority": "skip", "coverage": { "level": "body_partial", "label": "已检查正文中支撑判断的指定章节", "source_version": "arXiv:2610.12429v1", "inspected_sections": [ "Introduction", "Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114", "07 October 2026", "References", "I End Matter", "I. Data, QNM filter and the direct wave", "II. Numerical Teukolsky echoes", "III. The search on GW250114 and tests of the bound", "IV. Forecast for future detectors", "V. Reflectivity and Echoes from ECOs in the Teukolsky framework", "Instructions for reporting errors" ], "source_references": [ { "kind": "arxiv_source_package", "url": "https://export.arxiv.org/src/2610.12429v1", "locator": "Introduction; Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114; 07 October 2026; References; I End Matter; I. Data, QNM filter and the direct wave; II. Numerical Teukolsky echoes; III. The search on GW250114 and tests of the bound; IV. Forecast for future detectors; V. Reflectivity and Echoes from ECOs in the Teukolsky framework; Instructions for reporting errors", "description": "Complete, revision-matched arXiv TeX source package", "sha256": "05f8dd4fe10e8e7795f1bbdf65e3fe9bdcc73102497797faab86130084f41e44" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:44:21.805Z", "reason": "论文聚焦于利用双黑洞并合引力波事件 GW250114 检验并合残骸近视界反射率及引力波回声（echoes），探讨奇异致密天体（ECO）与黑洞视界量子物理。该研究属于纯引力波物理与经典/量子引力理论检验，与高能瞬变天体物理（FRB/PRS、超新星中心引擎、激波破越与周星相互作用、相对论喷流及电磁对应体）无实质联系。", "result": "基于 GW250114 数据搜寻引力波回声未见显著偏离黑洞无毛定理的信号（贝叶斯因子 $\\ln\\mathcal{B} = -2.9$），在 $90\\%$ 可信度下测得视界反射率上限 $|\\mathcal{R}_s| < 0.059$（均匀先验）及 $< 0.073$（复平面均匀先验），对应反射能量比例上限 $|\\mathcal{R}_s|^2 < 3.5 \\times 10^{-3}$（$<0.4\\%$）。", "reading_entry": "III. The search on GW250114 and tests of the bound", "problem": "常规黑洞准正则模（QNM）振铃主要反映光环处的引力势峰，对近视界处可能存在的量子微观结构或奇异天体表面反射不敏感；需要寻找由跌落波（直接波 DW）反射产生并穿透势垒的引力波回声，以直接检验视界反射率的零假设。", "method": "利用自旋权重 $s=-2$ 的 Teukolsky 方程结合膜范式（Membrane paradigm）外推 ECO 反射边界条件，采用有理滤波器 $F(\\omega)=\\prod_{n=0}^{2}\\frac{\\omega-\\omega_{22n}}{\\omega-\\omega_{22n}^{*}}\\frac{\\omega+\\omega_{22n}^{*}}{\\omega+\\omega_{22n}}$ 滤除准正则模，构建直接波与数值 Teukolsky 回声模型，并在高斯似然下对 GW250114 的 H1 与 L1 探测器数据开展联合贝叶斯参数估计与模拟注入分析。", "assumptions": [], "limits": [], "citation_leads": [ "Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114: “Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114”", "III. The search on GW250114 and tests of the bound: “The search on GW250114 and tests of the bound”", "V. Reflectivity and Echoes from ECOs in the Teukolsky framework: “Reflectivity and Echoes from ECOs in the Teukolsky framework”", "I. Data, QNM filter and the direct wave: “Data, QNM filter and the direct wave”" ], "research_progress": "首次利用在 GW250114 中识别出的直接波作为已知输入开展回声搜寻，将视界固有距离探索范围推进至普朗克尺度（$10^{-41} \\lesssim d_s/M_{\\rm f} \\lesssim 10^{-1}$），给出了目前近视界反射率最严格的直接观测上限 $|\\mathcal{R}_s| < 0.059$。", "figures": [ { "url": "/arxiv-figures/2610.12429/fig1_schematic.png", "caption": "Figure 1: Schematic spacetime picture of the first echo. Radiation from the plunging source (star) reaches the observer through the barrier as the DW (blue). Radiation emitted toward the horizon, ( + ) (+) , and the part of the outgoing radiation reflected by the barrier, ( − ) (-) ( ℛ BH \\mathcal{R}^{\\rm BH} ), are reflected at the surface ( ℛ s \\mathcal{R}_{s} ) and cross the barrier outward as the echo. The barrier modulates their frequency content. The ( − ) (-) path is delayed by exactly Δ ​ t = − 2 ​ r ∗ s \\Delta t=-2r_{*}^{s} with respect to the DW.", "label": "Fig. 1", "category": "theoretical", "category_badge": "物理模型示意图", "is_schematic": true } ], "unresolved_checks": [ "未进行独立同行评审或逐项复算。", "源文件中的图像未进行视觉核对。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } }, { "arxiv_id": "2610.12462", "revision": 1, "title": "Disk Structure May Determine AGN Variability and Explain the Accretion Disk Size Problem: No Broad Line Region Required", "abstract": "Variability is a crucial probe of active galactic nuclei (AGN) disks, but the impact of the structure and internal physics of the disk on this variability is poorly understood. We perform 3D multi-frequency radiation magnetohydrodynamic simulations of the $1300-5940~\\rmÅ$ emitting region of an AGN disk. This turbulent disk simulation happens to stochastically have different disk thickness above and below the midplane. Light curves emitted from the thin top of the disk are broadly consistent with traditional variability models, where the X-ray irradiation emitted from the corona is the main driver of variability in UV-optical light curves. Conversely, the UV-optical light curves emitted from the thicker bottom of the disk are not strongly correlated with the X-ray light curve and have disk continuum reverberation mapping lags that are $3-5\\times$ longer than the light travel time. While these features are inconsistent with traditional variability models, they are in good agreement with numerous recent observations. Our simulations allow us to interpret these recent observations with a new model for AGN disks, where the thicker disk leads to greater X-ray absorption, less X-ray reprocessing at larger disk radii, and a stronger signal from intrinsic variability driven by fluctuations in the AGN disk. In our simulations, we can measure the inflow timescale of these fluctuations as a long lag between light curves emitted from different disk radii. Understanding how disk structure impacts AGN variability and reverberation mapping can allow us to predict the thickness of AGN disks using UV-optical AGN light curves.", "published": "2026-10-08T17:59:49Z", "updated": "2026-10-08T17:59:49Z", "authors": [ "Amy Secunda", "Yan-Fei Jiang", "Jenny E. Greene" ], "url": "https://arxiv.org/abs/2610.12462v1", "categories": [ "astro-ph.HE", "astro-ph.GA" ], "primary_category": "astro-ph.HE", "analysis": { "arxiv_id": "2610.12462", "revision": 1, "status": "ready", "source_fingerprint": "8156b8ff8488bc9bd51e9c0345019cda133e5ded8e250ee33860b679bb8dbb64", "priority": "skip", "coverage": { "level": "abstract_only", "label": "仅依据 arXiv 摘要筛选，未检查正文", "source_version": "arXiv:2610.12462v1", "inspected_sections": [ "Abstract" ], "source_references": [ { "kind": "arxiv_abstract", "url": "https://arxiv.org/abs/2610.12462v1", "locator": "Abstract", "description": "arXiv abstract in the discovery record" } ] }, "analysis": { "origin": "ai", "model": "gpt-6-luna", "analyzed_at": "2026-10-09T11:30:44.167Z", "reason": "论文聚焦活动星系核吸积盘结构与紫外—光学变异、连续谱回响时延；摘要未显示其与所列高能瞬变、致密天体高能观测或相关环境研究有实质联系。", "result": "未能从已检查材料中核实论文结果。", "reading_entry": "摘要", "problem": "未能从已检查材料中核实论文问题陈述。", "method": "未能从已检查摘要中核实方法说明。", "assumptions": [], "limits": [], "citation_leads": [ "Abstract: “We perform 3D multi-frequency radiation magnetohydrodynamic simulations of the $1300-5940~\\rmÅ$ emitting region of an AGN disk.”" ], "research_progress": "已检查材料不足以判断相对既有工作的增量。", "figures": [], "unresolved_checks": [ "未进行独立同行评审或逐项复算。" ], "potential_lineage": { "status": "no_match", "reason": "自动筛选未建立论文与组内 Work 的科学关系。", "candidates": [] }, "prerequisite_works": [] } } } ] }, "knowledge_points": [] }