Relativistic equation of state of nuclear matter for the supernova explosion and the birth of neutron stars

Details Relativistic equation of state of nuclear matter for the supernova explosion and the birth of neutron stars Relativistic equation of state of nuclear matter for the supernova explosion and the birth of neutron stars

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..700s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 700-718

Physics

Nuclear Physics

75

Equations Of State, Neutron Stars, Nuclei (Nuclear Physics), Relativity, Star Formation, Stellar Interiors, Supernovae, Field Theory (Physics), Leptons, Neutrons, Nuclear Reactions, Protons

Scientific paper

We provide a relativisitic equation of state for supernovae and neutron stars using the relativistic mean field theory. The parameters in the theory are extracted from the properties of finite nuclei in the wide mass range in the periodic table including neutron-rich nuclei. We explore properties of high-density nuclear matter under various environments, such as various proton mixing ratios and temperatures realized in the supernova explosion and the birth of neutron stars. Properties of asymmetric nuclear matter with arbitrary proton fractions are compared with the parameterized equation of state, which has been used in the systematic studies of supernova explosions. We study the equation of state of high-density and high-temperature matter for neutron stars and supernovae, containing leptons under the chemical equilibrium condition. The proton fraction of neturon star matter turns out to be large enough due to the large symmetry energy to allow the direct Urca process which leads to the rapid cooling of neutron stars.

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