Hot Strange Stars II. Numerical Results and Discussion

The equilibrium states of hot strange stars has been studied. The equation of state of hot strange quark matter is determined based on the bag model MIT. It is shown that the dependencies mass-central density and radius-mass of hot strange stars is weakly depended on the central temperature T in the region 0 < T < 100 Mev. In contrast to this, the mass of the strange star with a fixed baryonic charge decreases significantly with the decrease in temperature. The strange stars with a baryonic charge N < 1.83·10⁵⁷ during cooling only shrink. If N > 2.02·10⁵⁷ they only expand. In case 1.83·10⁵⁷ < N < 2.02·10⁵⁷ depending on the initial temperature the strange stars at the beginning of cooling may first expand and then shrink, or shrink only. For hot strange stars the weight of the thermal energy and non-zero density of quark matter at zero pressure are of fundamental significance.