paper

Beta equilibrium under neutron star merger conditions

arXiv:2108.03324 · doi:10.3390/universe7110399

Abstract

We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range MeVMeV. We improve on previous work by using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models. We find that the nonzero-temperature correction can be of order to MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of or more if it is neglected.

arXiv commentv2: version published in Universe, minor changes in nomenclature, 20 pages, 14 figures v3: corrected typo in Eq.(C19)

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