Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics

In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dyn...

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Published inAstrophysical journal. Letters Vol. 967; no. 1; p. L14
Main Authors Most, Elias R., Haber, Alexander, Harris, Steven P., Zhang, Ziyuan, Alford, Mark G., Noronha, Jorge
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.05.2024
IOP Publishing
American Astronomical Society
Subjects
Binary stars
Collision dynamics
Flavors
Gravitational waves
Hydrodynamics
Neutrinos
Neutron stars
Nuclear astrophysics
Nuclear matter
Nuclear physics
Star mergers
Viscosity
Wave spectra
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ISSN2041-8205
2041-8213
DOI10.3847/2041-8213/ad454f

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Abstract In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dynamics during the collision by incorporating direct and modified Urca processes (in the neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. We demonstrate how weak-interaction-driven bulk viscosity in postmerger simulations can emerge and assess the bulk viscous dynamics of the resulting flow. We further place limits on the impact of the postmerger gravitational-wave strain. Our results show that weak-interaction-driven bulk viscosity can potentially lead to a phase shift of the postmerger gravitational-wave spectrum, although the effect is currently on the same level as the numerical errors of our simulation.
AbstractList In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dynamics during the collision by incorporating direct and modified Urca processes (in the neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. We demonstrate how weak-interaction-driven bulk viscosity in postmerger simulations can emerge and assess the bulk viscous dynamics of the resulting flow. We further place limits on the impact of the postmerger gravitational-wave strain. Our results show that weak-interaction-driven bulk viscosity can potentially lead to a phase shift of the postmerger gravitational-wave spectrum, although the effect is currently on the same level as the numerical errors of our simulation.
Abstract In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dynamics during the collision by incorporating direct and modified Urca processes (in the neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. We demonstrate how weak-interaction-driven bulk viscosity in postmerger simulations can emerge and assess the bulk viscous dynamics of the resulting flow. We further place limits on the impact of the postmerger gravitational-wave strain. Our results show that weak-interaction-driven bulk viscosity can potentially lead to a phase shift of the postmerger gravitational-wave spectrum, although the effect is currently on the same level as the numerical errors of our simulation.
In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dynamics during the collision by incorporating direct and modified Urca processes (in the neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. We demonstrate how weak-interaction-driven bulk viscosity in postmerger simulations can emerge and assess the bulk viscous dynamics of the resulting flow. We further place limits on the impact of the postmerger gravitational-wave strain. Our results show that weak-interaction-driven bulk viscosity can potentially lead to a phase shift of the postmerger gravitational-wave spectrum, although the effect is currently on the same level as the numerical errors of our simulation.
Author Alford, Mark G.
Zhang, Ziyuan
Haber, Alexander
Harris, Steven P.
Most, Elias R.
Noronha, Jorge
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  surname: Most
  fullname: Most, Elias R.
  organization: California Institute of Technology Walter Burke Institute for Theoretical Physics, Pasadena, CA 91125, USA
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  givenname: Alexander
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  surname: Haber
  fullname: Haber, Alexander
  organization: Washington University in St. Louis Physics Department, St. Louis, MO 63130​, USA
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  givenname: Steven P.
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  surname: Harris
  fullname: Harris, Steven P.
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  givenname: Ziyuan
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  surname: Zhang
  fullname: Zhang, Ziyuan
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  givenname: Jorge
  orcidid: 0000-0002-9817-0272
  surname: Noronha
  fullname: Noronha, Jorge
  organization: University of Illinois at Urbana-Champaign, Urbana Illinois Center for Advanced Studies of the Universe & Department of Physics, IL 61801, USA
BackLink https://www.osti.gov/biblio/2352306$$D View this record in Osti.gov
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Snippet In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium....
In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor (β-)equilibrium....
Abstract In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β...
In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ( β -)equilibrium....
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StartPage L14
SubjectTerms Binary stars
Collision dynamics
Flavors
Gravitational waves
Hydrodynamics
Neutrinos
Neutron stars
Nuclear astrophysics
Nuclear matter
Nuclear physics
Star mergers
Viscosity
Wave spectra
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Title Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics
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