Relativistic equation of state for supernova and neutron star

Details Relativistic equation of state for supernova and neutron star Relativistic equation of state for supernova and neutron star

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003nupha.721.1048s&link_type=abstract

Nuclear Physics A, Volume 721, p. C1048-C1051.

Physics

Nuclear Physics

1

Scientific paper

We construct the equation of state (EOS) of nuclear matter at finite temperature and density with various proton fractions within the relativistic mean field (RMF) theory for use in supernova simulations. The properties of nuclear matter with both uniform and non-uniform distributions are studied consistently. We tabulate the outcome in terms of the pressure, free energy, entropy, etc. at a sufficiently large number of mesh points in the density range ϱB = 105.1 ~ 1015.4g/cm3, the temperature range T = 0 ~ 100 MeV and the proton fraction range Yp = 0 ~ 0.56 to be used for supernova simulations. We also discuss the EOS of neutron star matter at zero temperature in a wide density range including hyperons.

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