Evolution of relativistic thin discs with a finite ISCO stress – II. Late time behaviour

• Published in: Monthly notices of the Royal Astronomical Society Vol. 489; no. 1; pp. 143 - 152
• Main Authors: Mummery, Andrew, Balbus, Steven A
• Format: Journal Article
• Language: English
• Published: 11.10.2019
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stz2142

ABSTRACT We present solutions to the relativistic thin disc evolutionary equation using a modified description of the mean fluid flow within the disc. The model takes into account the effects of sub-circular velocities in the innermost disc regions, and resolves otherwise unsustainable behaviour present in simple finite innermost stable circular orbit (ISCO) stress disc models. We show that the behaviour of a relativistic thin disc evolving with a finite ISCO stress is comprised of three distinct stages which join the ordinarily distinct finite and vanishing ISCO stress solutions into a fully continuous model parametrization. The most important prediction of our model is the existence of an intermediate stage of ‘stalled accretion’, controlled by a single dimensionless parameter. The hallmarks of this evolutionary phase appear to have been seen in General Relativistic MHD simulations as well as in the late time X-ray observations of tidal disruption events, but dedicated simulations and extended observations are needed for a deeper understanding.