Strongly asymmetric nuclear matter becomes unstable with respect to proton localization above a specific critical nuclear density. For equation of state of Akmal, Pandharipande and Ravenhall the Tolman-Oppenheimer-Volkoff equations were solved and the radius of the spherical shell of a neutron star within which proton localization takes place was found.
This paper investigates thermal properties of nuclear matter using the Friedman-Pandharipande- Ravenhall equation of state. Thermodynamic quantities such as internal energy, entropy and free energy are calculated both for symmetric and asymmetric nuclear matter for temperatures ranging up to 30 MeV. A change of free energy curvature indicates the liquid-gas phase transition in nuclear matter.
In this paper, our earlier approach to proton localization in neutron star matter to finite temperatures is extended. The Skyrme forces were chosen to describe interactions in nuclear matter. The dependence of threshold density on temperatures for proton localization was obtained and these results were compared with those calculated earlier for the Friedman-Pandharipande-Ravenhall potential.
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