GRRMHD Simulations of Tidal Disruption Event Accretion Disks around Supermassive Black Holes: Jet Formation, Spectra, and Detectability
GRRMHD Simulations of Tidal Disruption Event Accretion Disks around Supermassive Black Holes: Jet Formation, Spectra, and Detectability
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DOI：
10.1093/mnras/sty3134
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发表时间：
2018-11
影响因子：
4.8
通讯作者：
B. Curd;R. Narayan
中科院分区：
文献类型：
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作者：
B. Curd;R. Narayan
我们报告的结果，从广义相对论辐射MHD（GRRMHD）模拟的超爱丁顿黑洞（BH）吸积盘形成的潮汐破裂事件（TDE）的结果。我们考虑一个太阳质量的星星在一个温和的穿透轨道上被一个质量为10^6\，M\odot\$的超大质量BH破坏的基准情况，并考虑峰值回落率的时代。我们对模拟数据进行后处理以计算视角相关光谱。我们执行的吸积盘的动力学作为BH自旋和磁通量的函数的参数研究，并计算模型光谱作为观察者的视角的函数。我们还考虑基于模型光谱的检测限。我们发现，一个吸积盘与一个相对较弱的磁场周围的BH（所谓的SANE制度的吸积）不发射相对论性喷流，无论BH是旋转。这种模式合理地再现了非喷流TDE的几个观测特性。对于具有强磁场的非旋转BH（MAD区域）也是如此。我们的一个模拟有一个快速旋转的BH（自旋参数0.9）以及一个MAD吸积盘。这个模型发射了一个强大的相对论喷流，它是由BH自旋能量驱动的。它令人惊讶地再现了喷射的TDE Swift J1644+57的高能量发射和喷射结构。因此，喷射TDE可能对应于具有快速旋转BH和MAD吸积的TDE系统的子集。
We report results from general relativistic radiation MHD (GRRMHD) simulations of a super-Eddington black hole (BH) accretion disk formed as a result of a tidal disruption event (TDE). We consider the fiducial case of a solar mass star on a mildly penetrating orbit disrupted by a supermassive BH of mass $10^6 \, M_\odot$, and consider the epoch of peak fall back rate. We post-process the simulation data to compute viewing angle dependent spectra. We perform a parameter study of the dynamics of the accretion disk as a function of BH spin and magnetic flux, and compute model spectra as a function of the viewing angle of the observer. We also consider detection limits based on the model spectra. We find that an accretion disk with a relatively weak magnetic field around the BH (so-called SANE regime of accretion) does not launch a relativistic jet, whether or not the BH is rotating. Such models reasonably reproduce several observational properties of non-jetted TDEs. The same is also true for a non-rotating BH with a strong magnetic field (MAD regime). One of our simulations has a rapidly rotating BH (spin parameter 0.9) as well as a MAD accretion disk. This model launches a powerful relativistic jet, which is powered by the BH spin energy. It reproduces the high energy emission and jet structure of the jetted TDE Swift J1644+57 surprisingly well. Jetted TDEs may thus correspond to the subset of TDE systems that have both a rapidly spinning BH and MAD accretion.