Beta equilibrium under neutron star merger conditions

Mark G. Alford; Alexander Haber; Steven P. Harris; Ziyuan Zhang

doi:10.3390/universe7110399

Beta equilibrium under neutron star merger conditions

Mark G. Alford, Alexander Haber, Steven P. Harris, Ziyuan Zhang

Department of Physics

Research output: Contribution to journal › Article › peer-review

31 Scopus citations

Abstract

We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T < 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.

Original language	English
Article number	399
Journal	Universe
Volume	7
Issue number	11
DOIs	https://doi.org/10.3390/universe7110399
State	Published - Nov 2021

Keywords

Beta equilibration
Neutron star merger
Nuclear matter
Weak interaction

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title = "Beta equilibrium under neutron star merger conditions",

abstract = "We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T < 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.",

keywords = "Beta equilibration, Neutron star merger, Nuclear matter, Weak interaction",

author = "Alford, {Mark G.} and Alexander Haber and Harris, {Steven P.} and Ziyuan Zhang",

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T1 - Beta equilibrium under neutron star merger conditions

AU - Alford, Mark G.

AU - Haber, Alexander

AU - Harris, Steven P.

AU - Zhang, Ziyuan

PY - 2021/11

Y1 - 2021/11

N2 - We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T < 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.

AB - We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T < 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.

KW - Beta equilibration

KW - Neutron star merger

KW - Nuclear matter

KW - Weak interaction

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U2 - 10.3390/universe7110399

DO - 10.3390/universe7110399

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AN - SCOPUS:85118237850

SN - 2218-1997

VL - 7

JO - Universe

JF - Universe

IS - 11

M1 - 399

ER -

Beta equilibrium under neutron star merger conditions

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Keywords

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