Equation of state of neutron star matter and its warm extension with an interacting hadron resonance gas

被引：6

作者：

Fujimoto, Yuki ^{[1
]}

Fukushima, Kenji ^{[1
]}

Hidaka, Yoshimasa ^{[2
,3
,4
]}

Hiraguchi, Atsuki ^{[5
,6
]}

Iida, Kei ^{[6
]}

机构：

[1] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[2] KEK, Inst Particle & Nucl Studies, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan

[3] Grad Univ Adv Studies Sokendai, Tsukuba, Ibaraki 3050801, Japan

[4] RIKEN, RIKEN iTHEMS, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[5] Natl Yang Ming Chiao Tung Univ, Inst Phys, Hsinchu 30010, Taiwan

[6] Kochi Univ, Dept Math & Phys, Kochi 7808520, Japan

来源：

PHYSICS LETTERS B | 2022年 / 835卷

基金：

日本学术振兴会;

关键词：

STATISTICAL THERMODYNAMICS; QCD;

D O I：

10.1016/j.physletb.2022.137524

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We propose an interpolating equation of state that satisfies phenomenologically established boundary conditions in two extreme regimes at high temperature and low baryon density and at low temperature and high baryon density. We confirm that the hadron resonance gas model with the Carnahan-Starling excluded volume effect can reasonably fit the empirical equation of state at high density up to several times the normal nuclear density. We identify the onsets of strange particles and quantify the strangeness contents in dense matter. We finally discuss the finite temperature effects and estimate the thermal index Gamma(th) as a function of the baryon density, which should be a crucial input for the core-collapse supernova and the binary neutron star merger simulations. (c) 2022 The Author(s). Published by Elsevier B.V. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/).

引用

页数：8

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