Microscopic nuclear equation of state at finite temperature and stellar stability
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nucl-th
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finitetemperatureequationmicroscopicnuclearstabilitystatestellar
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A microscopic nuclear equation of state compatible with all current astrophysical constraints constructed within the Brueckner-Hartree-Fock formalism is presented and extended in a consistent way to finite temperature. The effects of finite temperature on the properties of neutron stars are studied in detail and a universal relation regarding stellar stability is proposed.
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