# Evolution of relativistic thin discs with a finite ISCO stress: I. Stalled accretion

## TL;DR

This paper models the evolution of relativistic thin accretion discs with finite stress at the ISCO, showing that such models produce light curves consistent with tidal disruption events and evolve over time toward traditional models.

## Contribution

It introduces solutions for relativistic thin discs with finite ISCO stress, revealing a shallow power law decay in light curves and their evolution over time.

## Key findings

- Light curves follow a shallow power law with index -11/14 for finite ISCO stress.
- Solutions indicate a prolonged relaxation period of the disc.
- Power law index evolves, eventually matching traditional zero ISCO stress models.

## Abstract

We present solutions to the relativistic thin disc evolutionary equation using an ${\alpha}$-model for the turbulent stress tensor. Solutions with a finite stress at the innermost stable circular orbit (ISCO) give rise to bolometric light curves with a shallow power law time dependence, in good agreement with those observed in tidal disruption events. A self-similar model based on electron scattering opacity, for example, yields a power law index of $-11/14$, as opposed to $-19/16$ for the case of zero ISCO stress. These solutions correspond to an extended period of relaxation of the evolving disc which, like the light curves they produce, is not sustainable indefinitely. Cumulative departures from the approximation of exact circular orbits cause the power law index to evolve slowly with time, leading eventually to the steeper fall-off associated with traditional zero ISCO stress models. These modified solutions are discussed in detail in a companion paper.