Hot neutron stars and their equation of state

Abstract

A set of microscopic, covariant density-functional, and non-relativistic Skyrme-type equations of state is employed to study the structure of purely nucleonic neutron stars at finite temperature. After examining the agreement with presently available astrophysical observational constraints, we find that the magnitude of thermal effects depends on the nucleon effective mass as well as on the stiffness of the cold equation of state. We evidence a fairly small but model-dependent effect of finite temperature on stellar stability that is correlated with the relative thermal pressure inside the star.

arXiv comment10 pages, 8 figures

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Cited by in corpus (8)

• Equations of state for hot neutron stars -- II. The role of exotic particle degrees of freedom
• Universal relations for rapidly rotating cold and hot hybrid star
• Microscopic nuclear equation of state at finite temperature and stellar stability
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• Investigating Possible Existence of Hyper-Heavy Nuclei in Neutron Star Environment
• New ab initio constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: II. Thermal response in the suprasaturation density domain
• Properties of rapidly rotating hot neutron stars within Brueckner theory