A new equation of state of supernova matter

Details A new equation of state of supernova matter A new equation of state of supernova matter

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26as...42..215e&link_type=abstract

Astronomy and Astrophysics Supplement Series, vol. 42, Nov. 1980, p. 215-226. Deutsche Forschungsgemeinschaft

Astronomy and Astrophysics

Astrophysics

36

Astrophysics, Equations Of State, Matter (Physics), Stellar Structure, Supernovae, Gravitational Collapse, Nuclear Binding Energy, Nucleon-Nucleon Interactions, Partitions (Mathematics), Weak Energy Interactions

Scientific paper

An equation of state of matter at high densities (greater than or equal to 10 to the 11th g/cu cm) and temperatures (greater than 5 x 10 to the 9th K) is presented which includes several important effects such as neutron and proton degeneracy as well as nucleon-nucleon interactions and nuclear excitations. Results are given for matter in both nuclear statistical equilibrium and beta-equilibrium for different values of entropy, density and temperature. The numerical computations have been performed mainly for these values of the parameters which can be expected in the interiors of collapsing massive stars and supernovae, but the method can just as well be applied to other astrophysical systems, e.g. hot neutron stars. In the present work it is assumed that nuclei obey Boltzmann statistics up to essentially nuclear matter density (approximately 2 x 10 to the 14th g/cu cm) and some effects due to their finite volume (e.g. excluded volume effects and Coulomb interactions) are neglected.

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