论文标题
连续拟合潮汐破坏事件的X射线光谱
Continuum-Fitting the X-ray Spectra of Tidal Disruption Events
论文作者
论文摘要
We develop a new model for X-ray emission from tidal disruption events (TDEs), applying stationary general relativistic ``slim disk'' accretion solutions to supermassive black holes (SMBHs) and then ray-tracing the photon trajectories from the image plane to the disk surface, including gravitational redshift, Doppler, and lensing effects self-consistently.我们同时并成功地适合了两个TDE的多epoch XMM-Newton X射线光谱：Asassn-14Li和Asassn-15OI。我们测试了Asassn-15OI的观察到的，意外的X射线亮度的解释，包括延迟的磁盘形成和通过后处理层可变的遮挡。我们提出了一种更适合数据的新机制：``slimming disk''场景，其中吸收到边缘磁盘上变慢，降低了磁盘高度，并将更多的X射线暴露于内部磁盘上，从时间上到达视线，从时间上看。 10^6m_ \ odot $。对于Asassn-14Li，SMBH质量为$ 10^{+1} _ { - 7} \ times 10^6m_ \ odot $，旋转为$> 0.3 $。对于这两个TDE，我们的拟合质量都与独立的估计一致。对于Asassn-14Li，外部质量约束的应用将我们的旋转约束缩小到$> 0.85 $。 Asassn-14Li的质量积聚速率缓慢衰减，$ \ propto t^{ - 1.1} $，也许是由于效率低下的碎屑循环。超过$ \ $ 1100天，它的SMBH已获得$ΔM\约0.17 m_ \ odot $，这意味着祖细胞质量为$> 0.34 m_ \ odot $，即没有“缺失能量问题”，这两个TDE都会降低了氢柱密度的范围，又有一个元素的特征，也有几个元素的数量，几乎没有一个米兰的元素。耗尽或去除遮盖的气体。
We develop a new model for X-ray emission from tidal disruption events (TDEs), applying stationary general relativistic ``slim disk'' accretion solutions to supermassive black holes (SMBHs) and then ray-tracing the photon trajectories from the image plane to the disk surface, including gravitational redshift, Doppler, and lensing effects self-consistently. We simultaneously and successfully fit the multi-epoch XMM-Newton X-ray spectra for two TDEs: ASASSN-14li and ASASSN-15oi. We test explanations for the observed, unexpectedly slow X-ray brightening of ASASSN-15oi, including delayed disk formation and variable obscuration by a reprocessing layer. We propose a new mechanism that better fits the data: a ``Slimming Disk'' scenario in which accretion onto an edge-on disk slows, reducing the disk height and exposing more X-rays from the inner disk to the sightline over time.For ASASSN-15oi, we constrain the SMBH mass to $4.0^{+2.5}_{-3.1} \times 10^6M_\odot$. For ASASSN-14li, the SMBH mass is $10^{+1}_{-7}\times 10^6M_\odot$ and the spin is $>0.3$. For both TDEs, our fitted masses are consistent with independent estimates; for ASASSN-14li, application of the external mass constraint narrows our spin constraint to $>0.85$. The mass accretion rate of ASASSN-14li decays slowly, as $\propto t^{-1.1}$, perhaps due to inefficient debris circularization. Over $\approx$1100 days, its SMBH has accreted $ΔM \approx 0.17 M_\odot$, implying a progenitor star mass of $> 0.34 M_\odot$, i.e., no ``missing energy problem.'' For both TDEs, the hydrogen column density declines to the host galaxy plus Milky Way value after a few hundred days, suggesting a characteristic timescale for the depletion or removal of obscuring gas.
