全球GRHD模拟中由流-流和流-盘相互作用形成和供给的潮汐扰动
Tidal Disruption Disks Formed and Fed by Stream-Stream and Stream-Disk Interactions in Global GRHD Simulations
摘要：
当一颗恒星靠近超大质量黑洞（BH）时，BH的潮汐力将其撕裂成一条细流，导致潮汐破裂事件（TDE）。在这项工作中，我们使用我们的GPU加速程序H-AMR研究了广义相对论流体力学（GRHD）中TDE的后中断阶段。我们进行了第一次基于网格的模拟的深穿透TDE（$β$ =7）与现实的系统参数：一个黑洞-恒星质量比$10^6$，抛物线恒星轨迹，和一个非零BH自旋。我们还进行了模拟的倾斜TDE的恒星轨道是倾斜的BH中平面。我们表明，对于我们对齐的TDE，吸积盘的形式，由于轨道能量的耗散与$\sim$ 20%的下落物质达到BH。耗散最初主要由暴力的自相交，后来由近心附近的流盘相互作用。自相交完全破坏了进入的气流，导致五个不同的自相交事件，间隔约12小时，并在吸积率燃烧。我们还发现，磁盘是偏心的，平均偏心率e $\approx$ 0.88。对于我们的倾斜TDE，我们发现只有部分的自相交，由于近心附近的节进动。虽然这些部分相交会将气体喷射出轨道平面，但仍会形成一个吸积盘，其吸积部分的物质与对齐的情况相似。这些结果具有重要的意义，磁盘的形成在现实的潮汐中断。例如，完全气流破裂引起的吸积速率的周期性可以解释Swift J1644+57的耀斑事件。
英文摘要：
When a star passes close to a supermassive black hole (BH), the BH's tidal forces rip it apart into a thin stream, leading to a tidal disruption event (TDE). In this work, we study the post-disruption phase of TDEs in general relativistic hydrodynamics (GRHD) using our GPU-accelerated code H-AMR. We carry out the first grid-based simulation of a deep-penetration TDE ($β$=7) with realistic system parameters: a black-hole-to-star mass ratio of $10^6$, a parabolic stellar trajectory, and a nonzero BH spin. We also carry out a simulation of a tilted TDE whose stellar orbit is inclined relative to the BH midplane. We show that for our aligned TDE, an accretion disk forms due to the dissipation of orbital energy with $\sim$20 percent of the infalling material reaching the BH. The dissipation is initially dominated by violent self-intersections and later by stream-disk interactions near the pericenter. The self-intersections completely disrupt the incoming stream, resulting in five distinct self-intersection events separated by approximately 12 hours and a flaring in the accretion rate. We also find that the disk is eccentric with mean eccentricity e$\approx$0.88. For our tilted TDE, we find only partial self-intersections due to nodal precession near pericenter. Although these partial intersections eject gas out of the orbital plane, an accretion disk still forms with a similar accreted fraction of the material to the aligned case. These results have important implications for disk formation in realistic tidal disruptions. For instance, the periodicity in accretion rate induced by the complete stream disruption may explain the flaring events from Swift J1644+57.
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