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Microscopic nuclear equation of state at finite temperature and stellar stability

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arxiv 2207.12146 v1 pith:GZTMDVDF submitted 2022-07-25 nucl-th

Hong-Ming Liu , Jing Zhang , Zeng-Hua Li , Jin-Biao Wei , G. F. Burgio , H.-J. Schulze This is my paper · ORCID
classification nucl-th
keywords finitetemperatureequationmicroscopicnuclearstabilitystatestellar
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A microscopic nuclear equation of state compatible with all current astrophysical constraints constructed within the Brueckner-Hartree-Fock formalism is presented and extended in a consistent way to finite temperature. The effects of finite temperature on the properties of neutron stars are studied in detail and a universal relation regarding stellar stability is proposed.

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