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