The equation of state near beta equilibrium for a collapsing stellar core

Details The equation of state near beta equilibrium for a collapsing stellar core The equation of state near beta equilibrium for a collapsing stellar core

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apjs...42..385m&link_type=abstract

Astrophysical Journal Supplement Series, vol. 42, Mar. 1980, p. 385-420. Research sponsored by the U.S. Department of Energy

Astronomy and Astrophysics

Astrophysics

10

Dense Plasmas, Equations Of State, Gravitational Collapse, Stellar Evolution, Stellar Structure, Thermodynamic Equilibrium, Electron Capture, Nuclear Particles, Particle Mass, Stellar Temperature, Temperature Dependence

Scientific paper

The composition and equation of state for the collapsing core of a massive star are calculated for temperatures in the range 5 billion to 500 billion K and densities in the range 50 billion to 50 trillion g/cu cm. The core is approximated by a noninteracting gas, including free nucleon degeneracy, high degrees of neutronization, and the thermal excitation of the nuclei. The conditions prior to and at beta equilibrium are calculated, and analytic expressions for the inhibition of the electron capture rates by neutrino degeneracy are obtained

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