Effects of self-gravity of the accretion disk around rapidly rotating black hole in long GRBs

TL;DR

This paper develops an analytical framework to study how the self-gravity of accretion disks influences the evolution of black holes in long GRBs, highlighting the importance of self-force effects during rapid mass accretion.

Contribution

It introduces a new analytical method to incorporate self-gravity effects of accretion disks in evolving Kerr black hole models for long GRBs.

Findings

Framework for self-gravity effects in accretion disks developed

Highlights importance of self-force during transient accretion events

Future numerical studies planned to validate the model

Abstract

We prescribe a method to study the effects of self-gravity of accretion disk around a black hole associated with long Gamma Ray Bursts (GRBs) in an evolving background Kerr metric. This is an extension to our previous work where we presented possible constraints for the final masses and spins of these astrophysical black holes. Incorporating the self-force of the accreting cloud around the black hole is a very important aspect due to the transient nature of the event, in which a huge amount of mass is accreted and changes the fundamental black hole parameters i.e. its mass and spin, during the process. Understanding of the GRBs engine is important because they are possible sources of high-energy particles and gravitational waves as most of the energy released from the dynamical evolution is in the form of gravitational radiation. Here, we describe the analytical framework we developed to employ in our numerical model. The numerical studies are planned for the future work.