Microscopic nuclear equation of state at finite temperature and stellar stability
arXiv:2207.12146 · doi:10.1103/PhysRevC.106.025801
Abstract
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.
9 pages, 7 figures
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- New Skyrme parametrizations to describe finite nuclei and neutron star matter with realistic effective masses