The effect of GREA on the gravitational collapse of neutron stars

TL;DR

This paper investigates how the General Relativistic Entropic Acceleration (GREA) framework influences neutron star collapse, revealing differences in mass-radius relations and implications for multimessenger astrophysics.

Contribution

It introduces the application of GREA to neutron star collapse, showing deviations from traditional models and providing new mass limits for neutron stars.

Findings

Final neutron star mass and radius differ by ~15% from standard models.

Minimum neutron star mass is approximately 1.1 solar masses.

Maximum neutron star mass is around 2.4 solar masses.

Abstract

General Relativistic Entropic Acceleration (GREA) gives a general framework in which to study multiple out-of-equilibrium phenomena in the context of general relativity, like the late accelerated expansion of the universe or the formation of galaxies and the large scale structure of the universe. Here we analyze the conditions for collapse of a star of degenerate neutrons in the presence of entropy production due to the gravitational collapse itself. We find that the final mass and radius of the neutron star differs from that obtained with the adiabatic Tolman-Oppenheimer-Volkoff equation by a factor of order 15\%. We also find that the minimum mass of a neutron star is $\sim 1.1\,M_\odot$ and the maximum mass around $2.4\,M_\odot$. We discuss the possible implications for the search and interpretation of binary coalescing systems like neutron stars and neutron star-black holes detectable via their multimessenger (gravitational and electromagnetic wave) emission upon merging.