论文标题
较轻的更柔和的柔和：$α_ {\ rm ox} $，X射线频谱状态和潮汐破坏事件中的爱丁顿比率之间的相关性
Fainter harder brighter softer: a correlation between $α_{\rm ox}$ , X-ray spectral state and Eddington ratio in tidal disruption events
论文作者
论文摘要
我们使用7 X-Ray明亮来源的样本探索潮汐破坏事件（TDE）的增生状态。为此，我们估计磁盘和电晕通过光谱建模对观察到的X射线发射的相对贡献，并评估X射线亮度（通过$α$ _OX，l $ _ {2 keV} $和f $ _ {edd，x} $）作为Eddington的功能。我们报告了$α$ _OX和f $ _ {edd，bol} $之间的强阳性相关性； f $ _ {edd，x} $和f $ _ {edd，uv} $;以及l $ _ {2 keV} $和f $ _ {edd，uv} $的反相关。高f $ _ {edd，bol} $的TDE具有热支配的X射线光谱和高（软）$α$ _ox，而低f $ _ {EDD，BOL} $的TDE显示出重要的幂律贡献，并且较低（硬）$α$ _ox。类似于X射线二进制文件和活动的银河系核，X射线光谱状态之间的过渡发生在f $ _ {EDD，bol} $ $ {\ lot} $ 0.03左右，尽管由于样本量较小，不确定性很大。我们的结果表明，X射线调查更有可能在低f $ _ {EDD，BOL} $下发现TDE，而光学调查对高爱丁顿的比率更为敏感。 X射线和光学选定的TDE具有不同的UV和X射线特性，在得出速率，光度和黑洞质量函数时应考虑到这些特性。在坚硬的状态下观察到最大的超级质量黑洞周围的TDE。这可能表明TDE进化速度更快，BHS更大。
We explore the accretion states of tidal disruption events (TDEs) using a sample of 7 X- ray bright sources. To this end, we estimate the relative contribution of the disk and corona to the observed X-ray emission through spectral modeling, and assess the X-ray brightness (through $α$_ox, L$_{2 keV}$ and f$_{Edd,X}$) as a function of the Eddington ratio. We report strong positive correlations between $α$_ox and f$_{Edd,bol}$; f$_{Edd,X}$ and f$_{Edd,UV}$ ; and an anti-correlation for L$_{2 keV}$ and f$_{Edd,UV}$. TDEs at high f$_{Edd,bol}$ have thermal dominated X-ray spectra and high (soft) $α$_ox, whereas those at low f$_{Edd,bol}$ show a significant power-law contribution and low (hard) $α$_ox. Similar to X-ray binaries and active galactic nuclei, the transition between X-ray spectral states occurs around f$_{Edd,bol}$ ${\approx}$ 0.03, although the uncertainty is large due to the small sample size. Our results suggest that X-ray surveys are more likely to discover TDEs at low f$_{Edd,bol}$, whereas optical surveys are more sensitive to TDEs at high Eddington ratios. The X-ray and optical selected TDEs have different UV and X-ray properties, which should be taken into account when deriving rates, luminosity and black hole mass functions. TDEs around the most massive supermassive black holes are observed in the hard state; this could indicate that TDE evolution is faster around more massive BHs.
