Equations of motion, initial and boundary conditions for GRB

TL;DR

This paper compares various approaches to modeling the optically thick adiabatic phase of gamma-ray bursts, emphasizing the importance of the rate equation and initial conditions for black hole fireballs.

Contribution

It provides a comparative analysis of different methods for modeling GRB phases and discusses the role of baryonic loading and initial conditions in these models.

Findings

Different approaches to GRB modeling are contrasted.

The importance of the rate equation in hydrodynamics is highlighted.

Constraints on initial conditions for black hole fireballs are derived.

Abstract

We compare and contrast the different approaches to the optically thick adiabatic phase of GRB all the way to the transparency. Special attention is given to the role of the rate equation to be self consistently solved with the relativistic hydrodynamic equations. The works of Shemi and Piran (1990), Piran, Shemi and Narayan (1993), Meszaros, Laguna and Rees (1993) and Ruffini, Salmonson, Wilson and Xue (1999,2000) are compared and contrasted. The role of the baryonic loading in these three treatments is pointed out. Constraints on initial conditions for the fireball produced by electro-magnetic black hole are obtained.