arXiv 2501.033352025-01-23astro-ph.HE

X射线准周期爆发源的时间分辨哈勃空间望远镜紫外观测

Time-resolved Hubble Space Telescope UV observations of an X-ray quasi-periodic eruption source

Thomas Wevers, Muryel Guolo, Sean Lockwood, Andrew Mummery, Dheeraj R. Pasham, Riccardo Arcodia

备注：: 11 pages and 4 figures; accepted for publication in ApJ Letters
DOI：: 10.3847/2041-8213/adace9

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AI总结：

本研究通过协调的哈勃空间望远镜和XMM-Newton观测，发现X射线准周期爆发源eRO-QPE2的紫外发射来自致密吸积盘，排除了经典AGN盘模型，支持潮汐瓦解事件起源。

摘要：

X射线准周期爆发（QPEs）是邻近星系核中一种新颖的变率模式，其起源尚不清楚。它们的多波长特性受到的限制很少，因为研究几乎完全集中在X射线波段。在此，我们报告了对目前已知周期最短的X射线QPE源eRO-QPE2进行的时间分辨、协调的哈勃空间望远镜远紫外和XMM-Newton X射线观测。我们探测到一个明亮的紫外点源（$L_{\rm FUV} \approx {\rm few} \times 10^{41}$ erg s$^{-1}$），其在X射线爆发和宁静阶段之间未显示出统计显著的变率。该发射不太可能由核星团中的年轻恒星族提供能量。X射线到紫外的光谱能量分布可以由一个致密吸积盘（$R_{\rm out} = 343^{+202}_{-138} \\ R_{\rm g}$）来描述。这种致密盘与活动星系核中的典型盘不相容，但在恒星被潮汐瓦解后自然形成。我们的结果排除了（针对eRO-QPE2的）涉及i）经典AGN吸积盘和ii）完全没有吸积盘的模型。对于轨道体模型，由时间特性推导出的预期半径将自然导致准球形和偏心轨迹的盘-轨道体相互作用。我们推断黑洞质量为log$_{10}(M_{\rm BH}) = 5.9 \pm 0.3$ M$_{\odot}$，爱丁顿比率为0.13$^{+0.18}_{-0.07}$；结合致密外半径，这与现有的盘不稳定性模型不一致。在考虑宁静盘发射后，我们限制爆发成分的X射线与远紫外光度之比为$L_{\rm X} / L_{\rm FUV} > 16-85$（取决于内禀消光）。

英文摘要：

X-ray quasi-periodic eruptions (QPEs) are a novel mode of variability in nearby galactic nuclei whose origin remains unknown. Their multi-wavelength properties are poorly constrained, as studies have focused almost entirely on the X-ray band. Here we report on time-resolved, coordinated Hubble Space Telescope far ultraviolet and XMM-Newton X-ray observations of the shortest period X-ray QPE source currently known, eRO-QPE2. We detect a bright UV point source ($L_{\rm FUV} \approx {\rm few} \times 10^{41}$ erg s$^{-1}$) that does not show statistically significant variability between the X-ray eruption and quiescent phases. This emission is unlikely to be powered by a young stellar population in a nuclear stellar cluster. The X-ray-to-UV spectral energy distribution can be described by a compact accretion disk ($R_{\rm out} = 343^{+202}_{-138} \ R_{\rm g}$). Such compact disks are incompatible with typical disks in active galactic nuclei, but form naturally following the tidal disruption of a star. Our results rule out models (for eRO-QPE2) invoking i) a classic AGN accretion disk and ii) no accretion disk at all. For orbiter models, the expected radius derived from the timing properties would naturally lead to disk-orbiter interactions for both quasi-spherical and eccentric trajectories. We infer a black hole mass of log$_{10}(M_{\rm BH}) = 5.9 \pm 0.3$ M$_{\odot}$ and Eddington ratio of 0.13$^{+0.18}_{-0.07}$; in combination with the compact outer radius this is inconsistent with existing disk instability models. After accounting for the quiescent disk emission, we constrain the ratio of X-ray to FUV luminosity of the eruption component to be $L_{\rm X} / L_{\rm FUV} > 16-85$ (depending on the intrinsic extinction).

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