Threshold Temperature for Neutron-Star Emergence in a Gravitational Thermodynamic Framework

TL;DR

This paper reformulates the emergence of neutron stars within a gravitational thermodynamic framework, deriving characteristic temperature thresholds using entropy principles and hydrostatic equilibrium equations.

Contribution

It introduces a novel thermodynamic threshold approach to neutron-star emergence, combining entropy functional formulation with classical hydrostatic and redshift effects.

Findings

Derived four characteristic temperature scales for neutron stars.

Provided explicit TOV and Fermi-gas formulae within the thermodynamic context.

Established thermodynamic consistency relations for compact objects.

Abstract

Motivated by the entropy-functional formulation of emergent gravity, in which spacetime is endowed with a thermodynamic entropy that, upon extremization, yields the Einstein field equations, we reformulate the onset of a neutron star as a bulk gravitational-thermodynamic threshold problem. By combining the Jacobson-Padmanabhan perspective of gravity as an equation of state with Tolman redshift, Tolman-Oppenheimer-Volkoff hydrostatics, and a bulk binding versus thermal energy balance, we derive four characteristic temperature scales for a static compact object: the Newtonian virial threshold, the redshifted threshold as observed at infinity, the degenerate-matter threshold, and the surface screen temperature.The paper supplies a mathematically expanded derivation, explicit TOV and Fermi-gas formulae, and thermodynamic consistency relations.