“School of Physics”
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| Paper IPM / P / 6792 |
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| Abstract: | |||||
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Free energy per nucleon, nucleonic effective masses, proton fraction,
and the equation of state are calculated for hot neutron star matter.
Modern AV18 potential is employed in our calculations, together
with the older AV14 potential for the sake of comparison.
It is shown that the proton fraction decreases as the neutron star
matter cools down. It turns out that the AV18 equation of state
is considerably stiffer than that of the AV14 potential.
The polytropic behavior of the P(ρ) relation and the non-existence
of phase transition are also pointed out.
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