Microscopic nuclear equation of state at finite temperature and stellar stability

Hong-Ming Liu (刘宏铭), Jing Zhang (张晶), Zeng-Hua Li (李增花), Jin-Biao Wei (魏金标), G. F. Burgio, and H.-J. Schulze
Phys. Rev. C 106, 025801 – Published 3 August 2022

Abstract

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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  • Received 6 May 2022
  • Accepted 20 July 2022

DOI:https://doi.org/10.1103/PhysRevC.106.025801

©2022 American Physical Society

Physics Subject Headings (PhySH)

Nuclear Physics

Authors & Affiliations

Hong-Ming Liu (刘宏铭)1, Jing Zhang (张晶)1, Zeng-Hua Li (李增花)1,*, Jin-Biao Wei (魏金标)2, G. F. Burgio3, and H.-J. Schulze3

  • 1Institute of Modern Physics, Key Laboratory of Nuclear Physics and Ion-Beam Application, MOE, Fudan University, Shanghai 200433, People's Republic of China
  • 2School of Mathematics and Physics, China University of Geosciences, Lumo Road 388, 430074 Wuhan, China
  • 3Istituto Nazionale di Fisica Nucleare, Sezione di Catania, Dipartimento di Fisica, Universitá di Catania, Via Santa Sofia 64, 95123 Catania, Italy

  • *zhli09@fudan.edu.cn

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Vol. 106, Iss. 2 — August 2022

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