We demonstrate that the compact, thick disc formed in a tidal disruption event may be unstable to non-axisymmetric perturbations in the form of the Papaloizou-Pringle instability. We show this can lead to rapid redistribution of angular momentum that can be parametrized in terms of an effective Shakura-Sunyaev α parameter. For remnants that have initially weak magnetic fields, this may be responsible for driving mass accretion prior to the onset of the magnetorotational instability. For tidal disruptions around a 106 M☉ black hole, the measured accretion rate is super-Eddington but is not sustainable over many orbits. We thus identify a method by which the torus formed in tidal disruption event may be significantly accreted before the magnetorotational instability is established.
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- February 2018
- accretion discs;
- black hole physics;
- Astrophysics - High Energy Astrophysical Phenomena
- 9 pages, 10 figures, accepted for publication in MNRAS. Movies of simulations available at https://youtu.be/kBLAjY8n9vI and https://youtu.be/F8F0tmLbX38