equilibrium in neutron-star mergers [Beta equilibrium in neutron star mergers]
Abstract
Here, we show that the commonly used criterion for β equilibrium in neutrino-transparent dense nuclear matter becomes invalid as temperatures rise above 1 MeV. Such temperatures are attained in neutron-star mergers. By numerically computing the relevant weak-interaction rates we find that the correct criterion for β equilibrium requires an isospin chemical potential that can be as large as 10–20 MeV, depending on the temperature at which neutrinos become trapped.
- Publication Date:
- Research Org.:
- Washington Univ. in St. Louis, St. Louis, MO (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP)
- OSTI Identifier:
- 1489124
- Alternate Identifier(s):
- OSTI ID: 1489064
- Grant/Contract Number:
- FG02-05ER41375
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review C
- Additional Journal Information:
- Journal Volume: 98; Journal Issue: 6; Related Information: See Supplemental Material at http://link.aps.org/supplemental/10.1103/PhysRevC.98.065806 for tabulated data presented in our figures.; Journal ID: ISSN 2469-9985
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; 79 ASTRONOMY AND ASTROPHYSICS; Beta equilibrium; Urca process; neutron star; equation of state; Fermi surface
Citation Formats
Alford, Mark G., and Harris, Steven P. β equilibrium in neutron-star mergers [Beta equilibrium in neutron star mergers]. United States: N. p., 2018.
Web. doi:10.1103/PhysRevC.98.065806.
Alford, Mark G., & Harris, Steven P. β equilibrium in neutron-star mergers [Beta equilibrium in neutron star mergers]. United States. https://doi.org/10.1103/PhysRevC.98.065806
Alford, Mark G., and Harris, Steven P. Fri .
"β equilibrium in neutron-star mergers [Beta equilibrium in neutron star mergers]". United States. https://doi.org/10.1103/PhysRevC.98.065806. https://www.osti.gov/servlets/purl/1489124.
@article{osti_1489124,
title = {β equilibrium in neutron-star mergers [Beta equilibrium in neutron star mergers]},
author = {Alford, Mark G. and Harris, Steven P.},
abstractNote = {Here, we show that the commonly used criterion for β equilibrium in neutrino-transparent dense nuclear matter becomes invalid as temperatures rise above 1 MeV. Such temperatures are attained in neutron-star mergers. By numerically computing the relevant weak-interaction rates we find that the correct criterion for β equilibrium requires an isospin chemical potential that can be as large as 10–20 MeV, depending on the temperature at which neutrinos become trapped.},
doi = {10.1103/PhysRevC.98.065806},
journal = {Physical Review C},
number = 6,
volume = 98,
place = {United States},
year = {Fri Dec 28 00:00:00 EST 2018},
month = {Fri Dec 28 00:00:00 EST 2018}
}
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Works referencing / citing this record:
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