Neutrino Trapping and Out-of-Equilibrium Effects in Binary Neutron-Star Merger Remnants

被引：12

作者：

Espino, Pedro Luis ^{[1
,2
]}

Hammond, Peter ^{[1
]}

Radice, David ^{[1
,3
,4
]}

Bernuzzi, Sebastiano ^{[5
]}

Gamba, Rossella ^{[5
]}

Zappa, Francesco ^{[5
]}

Micchi, Luis Felipe Longo ^{[5
]}

Perego, Albino ^{[6
,7
]}

机构：

[1] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[2] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[3] Penn State Univ, Dept Phys, University Pk, PA 16802 USA

[4] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[5] Friedrich Schiller Univ Jena, Theoret Phys Inst, D-07743 Jena, Germany

[6] Univ Trento, Dipartimento Fis, Via Sommar 14, I-38123 Trento, Italy

[7] Trento Inst Fundamental Phys & Applicat, INFN TIFPA, Via Sommar 14, I-38123 Trento, Italy

来源：

PHYSICAL REVIEW LETTERS | 2024年 / 132卷 / 21期

基金：

美国国家科学基金会;

关键词：

THERMODYNAMICS CONDITIONS; DYNAMICAL EJECTA; PHYSICAL MODELS; CORE-COLLAPSE; MASS EJECTION; DRIVEN WINDS; MATTER; NUCLEOSYNTHESIS; SIMULATIONS; AFTERMATH;

D O I：

10.1103/PhysRevLett.132.211001

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We study out-of-thermodynamic-equilibrium effects in neutron-star mergers with 3D general-relativistic neutrino-radiation large-eddy simulations. During mergers, the cores of the neutron stars remain cold (T similar to a few MeV) and out of thermodynamic equilibrium with trapped neutrinos originating from the hot collisional interface between the stars. However, within similar to 2 to 3 ms matter and neutrinos reach equilibrium everywhere in the remnant massive neutron star. Our results show that dissipative effects, such as bulk viscosity, if present, are only active for a short window of time after the merger.

引用

页数：6

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