发表机构
Massachusetts Institute of Technology; Institute for Advanced Study; Princeton University; Harvard University; New York University（麻省理工学院; 高等研究院; 普林斯顿大学; 哈佛大学; 纽约大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出联合光谱-时变框架，同时拟合QPE时变与宁静光谱，应用于GSN 069和eRO-QPE2，支持EMRI模型，但数据稀疏存在多解，需密集观测。
AI 中文摘要
准周期爆发（QPEs）是来自星系核的重复性X射线暂现源，可能由恒星质量轨道体在极端质量比旋近（EMRI）中反复与超大质量黑洞（SMBH）的吸积盘碰撞所致。在此图像中，爆发的到达时间编码了轨道及其相对论进动，而宁静态光谱能量分布（SED）则探测同一吸积盘和SMBH，为同一轨道-盘系统提供了两个独立的约束。我们提出了一个联合光谱-时变框架，利用这一优势，同时拟合基于Kerr测地线频率和翘曲盘几何的解析QPE时变模型，以及共享相同SMBH质量、自旋和盘参数的自辐照盘SED模型。我们将其应用于QPE源GSN 069和eRO-QPE2，表明在每一个源中，QPE时变和宁静态光谱可以同时重现，为这些系统中的EMRI模型和翘曲盘提供了间接支持。然而，鉴于两个源中稀疏的时变数据，两者均不承认唯一解。在eRO-QPE2中，我们识别出六个物理模式，它们能同样好地重现时变和SED，这促使更密集的观测活动以明确识别其中一个。我们的结果既展示了QPE光谱-时变作为SMBH、其吸积盘和轨道伴星的精密探针的前景，也展示了稀疏采样QPE时变的混叠微妙性。
英文摘要
Quasi-periodic eruptions (QPEs) are repeating X-ray transients from galactic nuclei potentially caused by a stellar-mass orbiter repeatedly colliding with the accretion disk of a supermassive black hole (SMBH) in an extreme mass-ratio inspiral (EMRI). In this picture, the eruption arrival times encode the orbit and its relativistic precessions, while the quiescent spectral energy distribution (SED) probes the same disk and SMBH, providing two independent constraints on the same orbit-disk system. We present a joint spectral-timing framework that takes advantage of this by simultaneously fitting an analytic QPE timing model built on Kerr geodesic frequencies and a warped disk geometry, coupled to a self-irradiated disk SED model sharing the same SMBH mass, spin, and disk parameters. We apply it to the QPE sources GSN 069 and eRO-QPE2, showing that the QPE timings and quiescent spectra can be reproduced simultaneously in each, providing circumstantial support for the EMRI model and warped disks in these systems. However, given the sparse timing data in both sources, neither admits a unique solution. In eRO-QPE2, we identify six physical modes which reproduce the timings and SED comparably well, motivating denser observing campaigns to identify one unambiguously. Our results demonstrate both the promise of QPE spectral-timing as a precision probe of SMBHs, their accretion disks, and orbiting companions, and the aliasing subtleties of sparsely sampled QPE timings.
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