Abstract
The equation of state (EOS) of dense supernova matter composed of protons, neutrons, and relativistic electrons is calculated within finite temperature Brueckner Goldstone approach with effective two-body Sussex interaction and compared with asymmetric nuclear matter. Thermal effect on the EOS is studied at temperature 5, 7, and 10 MeV. The EOS of supernova matter is found to be stiffer than the corresponding asymmetric nuclear matter equation of state as expected. Single particle properties like distribution functions and chemical potentials of proton, neutron, and electron are discussed for various values of electron fractions, densities, and temperatures. Distribution function is found to depend on Fermi kinetic energy of respective particles as well as on thermal energy. Chemical potential depends on number density of particles and temperature. It is also seen that the EOS for symmetric nuclear matter at low temperature has same order of magnitude with the recently extracted experimental values within the density range 0.35-0.56 fm{sup -3}.
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