Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers
Abstract
We discuss the bulk viscosity of hot and dense npeμ matter arising from weak-interaction direct Urca processes. We consider two regimes of interest: (a) the neutrino-transparent regime with T ≤ Ttr (Ttr ≃ 5 ÷ 10 MeV is the neutrino-trapping temperature); and (b) the neutrino-trapped regime with T ≥ Ttr. Nuclear matter is modeled in relativistic density functional approach with density-dependent parametrization DDME2. The maximum of the bulk viscosity is achieved at temperatures T ≃ 5 ÷ 6 MeV in the neutrino-transparent regime, then it drops rapidly at higher temperatures where neutrino-trapping occurs. As an astrophysical application, we estimate the damping timescales of density oscillations by the bulk viscosity in neutron star mergers and find that, e.g., at the oscillation frequency f = 10 kHz, the damping will be very efficient at temperatures 4 ≤ T ≤ 7 MeV where the bulk viscosity might affect the evolution of the post-merger object.
- Authors:
-
[1];
[2];
[3]
- Washington University, St. Louis, MO (United States)
- National Academy of Sciences, Byurakan (Armenia); Yerevan State University (Armenia)
- Frankfurt Institute for Advanced Studies (Germany); University of Wrocław (Poland)
- Publication Date:
- Research Org.:
- Washington University in St. Louis, MO (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP); German Research Foundation (DFG); Polish NCN
- OSTI Identifier:
- 2008328
- Grant/Contract Number:
- FG02-05ER41375; SE 1836/5-2; 2020/37/B/ST9/01937
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Particles
- Additional Journal Information:
- Journal Volume: 5; Journal Issue: 3; Journal ID: ISSN 2571-712X
- Publisher:
- MDPI
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; bulk viscosity; weak processes; npeμ matter; binary neutron star mergers; damping of density oscillations
Citation Formats
Alford, Mark, Harutyunyan, Arus, and Sedrakian, Armen. Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers. United States: N. p., 2022.
Web. doi:10.3390/particles5030029.
Alford, Mark, Harutyunyan, Arus, & Sedrakian, Armen. Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers. United States. https://doi.org/10.3390/particles5030029
Alford, Mark, Harutyunyan, Arus, and Sedrakian, Armen. Tue .
"Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers". United States. https://doi.org/10.3390/particles5030029. https://www.osti.gov/servlets/purl/2008328.
@article{osti_2008328,
title = {Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers},
author = {Alford, Mark and Harutyunyan, Arus and Sedrakian, Armen},
abstractNote = {We discuss the bulk viscosity of hot and dense npeμ matter arising from weak-interaction direct Urca processes. We consider two regimes of interest: (a) the neutrino-transparent regime with T ≤ Ttr (Ttr ≃ 5 ÷ 10 MeV is the neutrino-trapping temperature); and (b) the neutrino-trapped regime with T ≥ Ttr. Nuclear matter is modeled in relativistic density functional approach with density-dependent parametrization DDME2. The maximum of the bulk viscosity is achieved at temperatures T ≃ 5 ÷ 6 MeV in the neutrino-transparent regime, then it drops rapidly at higher temperatures where neutrino-trapping occurs. As an astrophysical application, we estimate the damping timescales of density oscillations by the bulk viscosity in neutron star mergers and find that, e.g., at the oscillation frequency f = 10 kHz, the damping will be very efficient at temperatures 4 ≤ T ≤ 7 MeV where the bulk viscosity might affect the evolution of the post-merger object.},
doi = {10.3390/particles5030029},
journal = {Particles},
number = 3,
volume = 5,
place = {United States},
year = {Tue Sep 06 00:00:00 EDT 2022},
month = {Tue Sep 06 00:00:00 EDT 2022}
}
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