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| Paper IPM / P / 7197 |
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| Abstract: | |
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A hot neutron star is born, within a short time after the
supernova explosion. The interior temperature of a neutron star,
at its birth, is of the order 20-50 MeV[1,2]. The properties of
the hot neutron star are clearly different from those of the cold
neutron star. Therefore, the calculation of these properties at
finite temperature is of special interest. We have calculated the properties of the newborn neutron star matter using the lowest order constrained variational method [3, 4, 5, 6, 7 and 8]. our results included the free energy per nucleon, effective masses of the proton and neutron, entropy per nucleon, proton fraction, and the equation of state. The effective mass of the proton was shown to be lower than that of the neutron. This result has an important implication for the occurrence of superfluidity inside neutron stars [9, 10]. The proton fraction was seen to decrease as the neutron star matter cools down. This result affects the cooling behavior and the details of superfluidity. The behavior of the Pρ relation did not irregularities which are signature of possible phase transitions. Download TeX format |
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