In relativistic mean field theory, a larger effective nucleon mass softens the supernova equation of state, yielding more compact proto-neutron stars, earlier black hole collapse, and higher-energy neutrino emission.
Influence of the symmetry energy on the birth of neutron stars and supernova neutrinos
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abstract
We study the influence of the symmetry energy of the equation of state on the thermal evolution of protoneutron stars and the properties of supernova neutrinos by the numerical simulations after the protoneutron stars are formed. As for the equation of state (EOS) of nuclear matter, we take two EOS's with different symmetry energies obtained by the relativistic mean field theory. We find the symmetry energy plays the essential role on the evolution of lepton profiles and the neutrino fluxes.
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Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects
In relativistic mean field theory, a larger effective nucleon mass softens the supernova equation of state, yielding more compact proto-neutron stars, earlier black hole collapse, and higher-energy neutrino emission.