Non-adiabatic radiative collapse of a relativistic star under different initial conditions

TL;DR

This paper investigates how different initial conditions and space-time geometries influence the non-adiabatic collapse of relativistic stars with heat dissipation, comparing homogeneous and inhomogeneous interior models.

Contribution

It introduces a comparative analysis of star collapse dynamics considering both homogeneous perfect fluids and inhomogeneous imperfect fluids with anisotropic pressure.

Findings

Collapse evolution depends solely on initial mass and size when shear-free.

Inhomogeneous geometries influence collapse behavior under specific conditions.

The study highlights the role of space-time geometry in stellar collapse processes.

Abstract

We examine the role of space-time geometry in the non-adiabatic collapse of a star dissipating energy in the form of radial heat flow, studying its evolution under different initial conditions. The collapse of a star with interior comprising of a homogeneous perfect fluid is compared with that of a star filled with inhomogeneous imperfect fluid with anisotropic pressure. Both the configurations are spherically symmetric, however, in the latter case, the physical space $t= constant$ of the configurations is assumed to be inhomogeneous endowed with spheroidal or pseudo-spheroidal geometry. It is observed that as long as the collapse is shear-free, its evolution depends only on the mass and size of the star at the onset of collapse.