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Paper IPM / P / 6857  


Abstract:  
The equation of state of hot neutrino opaque interior matter of
the neutron star and some of its properties such as the free
energy, effective mass, adiabatic index, and temperature are
calculated along both isothermal and isentropic paths with the
AV_{18} and AV_{14} potentials using the lowest
order constrained variational method. We have shown that the
calculated equation of state with the AV_{18} potential
is harder than with the AV_{14} potential. It is found
that there is no phase transition in the hot neutrino opaque
interior matter of the neutron star. We have shown that for all
values of density and entropy, the adiabatic index of neutron star
matter is greater than \frac {4}{3}. It is shown
that our calculated equations of state obey the causality
condition.
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