Equation of State of Supernova Matter | Zendy

Ryusuke Ogasawara | Zendy

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Equation of State of Supernova Matter

Author(s) -

Ryusuke Ogasawara

Publication year - 1985

Publication title -

progress of theoretical physics

Language(s) - English

Resource type - Journals

eISSN - 1347-4081

pISSN - 0033-068X

DOI - 10.1143/ptp.73.367

Subject(s) - physics , equation of state , supernova , nuclear matter , adiabatic process , fermi gamma ray space telescope , lepton , degenerate energy levels , nucleon , homogeneous , chandrasekhar limit , nuclear physics , fermi gas , phase transition , particle physics , condensed matter physics , quantum mechanics , astrophysics , white dwarf , thermodynamics , stars , electron

We have calculated the equation of state of the supernova matter for various values of lepton fraction YL and entropy per nucleon s by using the finite temperature Thomas-Fermi model of nuclei. The pressure is dominated by degenerate pressure of leptons and the adiabatic index r stays around 4/3. However, r decreases by the effect of the nuclear force at the very high density region. Although the nuclei melt at rather low density, about 10·gcmin this calculation, the comparison with a Hartree-Fock calculation reveals that the further investigation should be done to clarify the phase transition from nuclear phase of nucleon to homogeneous phase.

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