http://arxiv.org/abs/2008.04922
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 ($\beta=7$) 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 the first such simulation for 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, which is initially dominated by violent self-intersections, and later by stream-disk interactions near the pericenter, with $\sim20\%$ of the infalling material reaching the BH. The self-intersections completely disrupt the stream, resulting in five distinct self-intersection events separated by approximately 12 hours and a flaring in the accretion rate. For our tilted TDE, we find only partial self-intersections due to polar precession. Although they 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.
Z. Andalman, M. Liska, A. Tchekhovskoy, et. al.
Thu, 13 Aug 20
-897/67
Comments: Submitted to MNRAS, 20 pages, 23 figures, uses mnras.cls. Comments welcome. Movies available at this https URL
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