Equation of state for hot and dense n, p, e-mixture with zero charge density

Details Equation of state for hot and dense n, p, e-mixture with zero charge density Equation of state for hot and dense n, p, e-mixture with zero charge density

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....57..243e&link_type=abstract

Astronomy and Astrophysics, vol. 57, no. 1-2, May 1977, p. 243-249. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

24

Elementary Particles, Equations Of State, Gravitational Collapse, Nucleon-Nucleon Interactions, Supernovae, Baryons, Electron Density (Concentration), High Temperature Environments, Neutrons, Proton Density (Concentration), Thomas-Fermi Model

Scientific paper

An equation of state for matter (homogeneous charge-neutral mixture of electrons and interacting neutrons and protons) at the high temperatures and densities expected in a supernova core is calculated in a Thomas-Fermi approximation which simultaneously describes correctly the saturation properties of nuclear matter. It is shown that at densities of 10 to the 13th power to 10 to the 14th power and temperatures not exceeding 200 billion K, the attractive nuclear interaction lowers the pressure by up to a factor of five as compared with the results of previous works for pure neutron matter.

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