Proto-strange quark stars from density-dependent quark mass model

被引：9

作者：

Issifu, Adamu ^{[1
]}

da Silva, Franciele M. ^{[2
]}

Menezes, Debora P. ^{[2
]}

机构：

[1] Inst Tecnol Aeronaut, BR-12228900 Sao Jose Dos Campos, SP, Brazil

[2] Univ Fed Santa Catarina, Dept Fis, CFM, CP 476, BR-88040900 Florianopolis, SC, Brazil

来源：

EUROPEAN PHYSICAL JOURNAL C | 2024年 / 84卷 / 05期

基金：

巴西圣保罗研究基金会;

关键词：

EQUATION-OF-STATE; NEUTRON STARS; MATTER; EVOLUTION; DECONFINEMENT; TEMPERATURE; CONFINEMENT; BIRTH;

D O I：

10.1140/epjc/s10052-024-12828-0

中图分类号：

O412 [相对论、场论]; O572.2 [粒子物理学];

学科分类号：

摘要：

In this paper, we investigate the evolution of strange quark stars (SQS) from birth as proto-strange quark stars to maturity as stable SQSs at a zero temperature. We assume that self-bound free quarks form entirely the compact star and study its evolution through a series of snapshots using a density-dependent quark mass model. We consider beta \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\beta $$\end{document} -equilibrated stellar matter at two major stages of the star's evolution: neutrino trapped regime and neutrino transparent regime during the deleptonization and cooling processes of the star. We fix the entropy density per baryon and the lepton fraction to investigate the nuclear equation of state (EoS), particle distribution, temperature profile inside the star, sound velocity, polytropic index, and the structure of the star. Our results show that stars with higher neutrino concentrations are slightly more massive than the neutrino-poor ones along the evolution lines of the SQS. We obtain EoSs in agreement with the conformal boundary set through sound velocity, and also the 2 M circle dot \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_\odot $$\end{document} mass constraint for NSs was satisfied at all stages of the star's evolution.

引用

页数：16

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