Beta Equilibrium under Neutron Star Merger Conditions

We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1mEv < <i>T</i> ≲ 5 mEv. We improve on previous work using a consistent description of nuclear matter based on the IUF and...

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Autores principales:	Mark G. Alford, Alexander Haber, Steven P. Harris, Ziyuan Zhang
Formato:	article
Lenguaje:	EN
Publicado:	MDPI AG 2021
Materias:	nuclear matter neutron star merger beta equilibration weak interaction Elementary particle physics QC793-793.5
Acceso en línea:	https://doaj.org/article/e5dd0214faf3433b83333f2bb21933a0
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spelling	oai:doaj.org-article:e5dd0214faf3433b83333f2bb21933a02021-11-25T19:09:27ZBeta Equilibrium under Neutron Star Merger Conditions10.3390/universe71103992218-1997https://doaj.org/article/e5dd0214faf3433b83333f2bb21933a02021-10-01T00:00:00Zhttps://www.mdpi.com/2218-1997/7/11/399https://doaj.org/toc/2218-1997We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1mEv < <i>T</i> ≲ 5 mEv. We improve on previous work 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 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.Mark G. AlfordAlexander HaberSteven P. HarrisZiyuan ZhangMDPI AGarticlenuclear matterneutron star mergerbeta equilibrationweak interactionElementary particle physicsQC793-793.5ENUniverse, Vol 7, Iss 399, p 399 (2021)
institution	DOAJ
collection	DOAJ
language	EN
topic	nuclear matter neutron star merger beta equilibration weak interaction Elementary particle physics QC793-793.5
spellingShingle	nuclear matter neutron star merger beta equilibration weak interaction Elementary particle physics QC793-793.5 Mark G. Alford Alexander Haber Steven P. Harris Ziyuan Zhang Beta Equilibrium under Neutron Star Merger Conditions
description	We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1mEv < <i>T</i> ≲ 5 mEv. We improve on previous work 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 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.
format	article
author	Mark G. Alford Alexander Haber Steven P. Harris Ziyuan Zhang
author_facet	Mark G. Alford Alexander Haber Steven P. Harris Ziyuan Zhang
author_sort	Mark G. Alford
title	Beta Equilibrium under Neutron Star Merger Conditions
title_short	Beta Equilibrium under Neutron Star Merger Conditions
title_full	Beta Equilibrium under Neutron Star Merger Conditions
title_fullStr	Beta Equilibrium under Neutron Star Merger Conditions
title_full_unstemmed	Beta Equilibrium under Neutron Star Merger Conditions
title_sort	beta equilibrium under neutron star merger conditions
publisher	MDPI AG
publishDate	2021
url	https://doaj.org/article/e5dd0214faf3433b83333f2bb21933a0
work_keys_str_mv	AT markgalford betaequilibriumunderneutronstarmergerconditions AT alexanderhaber betaequilibriumunderneutronstarmergerconditions AT stevenpharris betaequilibriumunderneutronstarmergerconditions AT ziyuanzhang betaequilibriumunderneutronstarmergerconditions
_version_	1718410251206656000

Beta Equilibrium under Neutron Star Merger Conditions

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