Quark core neutron stars. Pt. 2

A Hartree-Fock calculation of the equation of state of quark matter interacting via quantum chromodynamics, is used to estimate rhosub(t) the density of the transition from nuclear matter to quark matter. The main result we get is that rhosub(t) is greater than the maximum central density of stable neutron stars, so that there is no quark matter in ordinary neutron stars. A secondary maximum of the (M,rho) curve is obtained, however at rho approx. equal to 1019 gcm 3 with a mass of M approx. 0.86 Msub(sun) corresponding to (probably unstable) quark stars. (orig.)