Abstract
One of the most intriguing possibilities to determine properties of the nuclear equation of state (EOS) is the astrophysical data of dense stars. Type II supernova and neutron stars offer two independent means of studying the nuclear EOS. Bethe1 has recently reviewed the nuclear physics of supernova. Neutron star EOS?s sample a different range of densities and isospin asymmetry than supernova. Thus these two situations yield related but not identical information about the EOS. It was hoped that the structure of neutron stars and their observed masses would constrain the wide variety of neutron star EOS’s.2 The only “hard” constraint is that the minimum maximum neutron star mass, M max, that an EOS must support is ~ 1.44 M ⊙,3,4 where M ⊙ is the solar mass. Recently several authors have concentrated on this aspect of the neutron star EOS.5–9 The common conclusion is that too “soft” of an EOS does not support a massive enough neutron star.
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