The birth of a ghost star

TL;DR

This paper develops an analytical model of a dissipative, self-gravitating fluid evolving into a ghost star, characterized by a zero-mass static configuration with negative energy density regions, and discusses possible observational implications.

Contribution

It introduces a novel analytical model of ghost star formation, incorporating dissipation, asymptotic behavior, and a cavity, expanding understanding of exotic stellar end states.

Findings

Model demonstrates the formation of a ghost star with negative energy density regions.

Includes a cavity surrounding the center due to specific radial distance variation.

Potential observational signatures of ghost stars are briefly discussed.

Abstract

We present a model of an evolving spherically symmetric dissipative self-gravitating fluid distribution which tends asymptotically to a ghost star, meaning that the end state of such a system corresponds to a static fluid distribution with vanishing total mass, and energy-density distribution which is negative in some regions of the fluid. The model is inspired in a solution representing a fluid evolving quasi-homologously and with vanishing complexity factor. However in order to satisfy the asymptotic behavior mentioned above, the starting solution has to be modified, as a consequence of which the resulting model only satisfies the two previously mentioned conditions, asymptotically. Additionally a condition on the variation of the infinitesimal proper radial distance between two neighboring points per unit of proper time is imposed, which implies the presence of a cavity surrounding the center. Putting together all these conditions we are able to obtain an analytical model depicting the emergence of a ghost star. Some potential observational consequences of this phenomenon are briefly discussed at the last section.