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The equation of state for matter with energy density above 2 x10^14 g/cm^3 isparametrized by P = kN^Gamma, where N is the number density, Gamma is theadiabatic index, and k a constant. Using this scheme to generate thousands ofmodels, together with data on neutron star masses, it is found, for a coreregion with a constant adiabatic index, that the central density must satisfy10^15 gm/cm^3 < rho_c < 10^16 gm/cm^3, with Gamma > 2.2. Further preliminaryresults indicate, based on the observed neutrino flux from supernova 1987a,that this number must be considerably higher, on the order of 3.5. Theseresults provide evidence for a hard equation of state in the cores of neutronstars.

Evidence for a hard equation of state in the cores of neutron stars