稠密天体物理燃烧火焰中夸克物质的电弱衰变

J. A. Rosero-Gil, G. Lugones
{"title":"稠密天体物理燃烧火焰中夸克物质的电弱衰变","authors":"J. A. Rosero-Gil, G. Lugones","doi":"10.1103/PhysRevC.103.055816","DOIUrl":null,"url":null,"abstract":"We study the weak interaction processes taking place within a combustion flame that converts dense hadronic matter into quark matter in a compact star. Using the Boltzmann equation we follow the evolution of a small element of just deconfined quark matter all along the flame interior until it reaches chemical equilibrium at the back boundary of the flame. We obtain the reaction rates and neutrino emissivities of all the relevant weak interaction processes without making any assumption about the neutrino degeneracy. We analyse systematically the role the initial conditions of unburnt hadronic matter, such as density, temperature, neutrino trapping and composition, focusing on typical astrophysical scenarios such as cold neutron stars, protoneutron stars, and post merger compact objects. We find that the temperature within the flame rises significantly in a timescale of 1 nanosecond. The increase in $T$ strongly depends on the initial strangeness of hadronic matter and tends to be more drastic at larger densities. Typical final values range between $20$ and $60 \\, \\mathrm{MeV}$. The nonleptonic process $u + d \\rightarrow u + s$ is always dominant in cold stars, but in hot object the process $u + e^{-} \\leftrightarrow d + {\\nu_e}$ becomes relevant, and in some cases dominant, near chemical equilibrium. The rates for the other processes are orders of magnitude smaller. We find that the neutrino emissivity per baryon is very large, leading to a total energy release per baryon of $2-64 \\, \\mathrm{MeV}$ in the form of neutrinos along the flame. We discuss some astrophysical consequences of the results.","PeriodicalId":8463,"journal":{"name":"arXiv: Nuclear Theory","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2020-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Electroweak decay of quark matter within dense astrophysical combustion flames\",\"authors\":\"J. A. Rosero-Gil, G. Lugones\",\"doi\":\"10.1103/PhysRevC.103.055816\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We study the weak interaction processes taking place within a combustion flame that converts dense hadronic matter into quark matter in a compact star. Using the Boltzmann equation we follow the evolution of a small element of just deconfined quark matter all along the flame interior until it reaches chemical equilibrium at the back boundary of the flame. We obtain the reaction rates and neutrino emissivities of all the relevant weak interaction processes without making any assumption about the neutrino degeneracy. We analyse systematically the role the initial conditions of unburnt hadronic matter, such as density, temperature, neutrino trapping and composition, focusing on typical astrophysical scenarios such as cold neutron stars, protoneutron stars, and post merger compact objects. We find that the temperature within the flame rises significantly in a timescale of 1 nanosecond. The increase in $T$ strongly depends on the initial strangeness of hadronic matter and tends to be more drastic at larger densities. Typical final values range between $20$ and $60 \\\\, \\\\mathrm{MeV}$. The nonleptonic process $u + d \\\\rightarrow u + s$ is always dominant in cold stars, but in hot object the process $u + e^{-} \\\\leftrightarrow d + {\\\\nu_e}$ becomes relevant, and in some cases dominant, near chemical equilibrium. The rates for the other processes are orders of magnitude smaller. We find that the neutrino emissivity per baryon is very large, leading to a total energy release per baryon of $2-64 \\\\, \\\\mathrm{MeV}$ in the form of neutrinos along the flame. We discuss some astrophysical consequences of the results.\",\"PeriodicalId\":8463,\"journal\":{\"name\":\"arXiv: Nuclear Theory\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2020-10-10\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"arXiv: Nuclear Theory\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1103/PhysRevC.103.055816\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv: Nuclear Theory","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1103/PhysRevC.103.055816","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0

摘要

我们研究了发生在燃烧火焰中将致密强子物质转化为致密恒星中夸克物质的弱相互作用过程。利用玻尔兹曼方程,我们沿着火焰内部跟踪刚定义的夸克物质的小元素的演化,直到它在火焰的后边界达到化学平衡。我们得到了所有相关弱相互作用过程的反应速率和中微子发射率,而不做任何关于中微子简并的假设。我们系统地分析了未燃烧强子物质的初始条件,如密度、温度、中微子俘获和组成,重点分析了典型的天体物理场景,如冷中子星、质子中子星和合并后致密天体。我们发现火焰内的温度在1纳秒的时间尺度内显著上升。$T$的增加很大程度上取决于强子物质的初始奇异性,并且在更大的密度下趋于更剧烈。典型的最终值范围在$20$和$60 \, \mathrm{MeV}$之间。非轻子过程$u + d \rightarrow u + s$在冷的恒星中总是占主导地位,但在热的物体中,过程$u + e^{-} \leftrightarrow d + {\nu_e}$变得相关,在某些情况下,在化学平衡附近占主导地位。其他过程的速率要小几个数量级。我们发现每个重子的中微子发射率非常大,导致每个重子沿火焰以中微子形式释放的总能量为$2-64 \, \mathrm{MeV}$。我们讨论了这些结果的一些天体物理学后果。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Electroweak decay of quark matter within dense astrophysical combustion flames
We study the weak interaction processes taking place within a combustion flame that converts dense hadronic matter into quark matter in a compact star. Using the Boltzmann equation we follow the evolution of a small element of just deconfined quark matter all along the flame interior until it reaches chemical equilibrium at the back boundary of the flame. We obtain the reaction rates and neutrino emissivities of all the relevant weak interaction processes without making any assumption about the neutrino degeneracy. We analyse systematically the role the initial conditions of unburnt hadronic matter, such as density, temperature, neutrino trapping and composition, focusing on typical astrophysical scenarios such as cold neutron stars, protoneutron stars, and post merger compact objects. We find that the temperature within the flame rises significantly in a timescale of 1 nanosecond. The increase in $T$ strongly depends on the initial strangeness of hadronic matter and tends to be more drastic at larger densities. Typical final values range between $20$ and $60 \, \mathrm{MeV}$. The nonleptonic process $u + d \rightarrow u + s$ is always dominant in cold stars, but in hot object the process $u + e^{-} \leftrightarrow d + {\nu_e}$ becomes relevant, and in some cases dominant, near chemical equilibrium. The rates for the other processes are orders of magnitude smaller. We find that the neutrino emissivity per baryon is very large, leading to a total energy release per baryon of $2-64 \, \mathrm{MeV}$ in the form of neutrinos along the flame. We discuss some astrophysical consequences of the results.
求助全文
通过发布文献求助,成功后即可免费获取论文全文。 去求助
来源期刊
自引率
0.00%
发文量
0
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
确定
请完成安全验证×
copy
已复制链接
快去分享给好友吧!
我知道了
右上角分享
点击右上角分享
0
联系我们:info@booksci.cn Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。 Copyright © 2023 布克学术 All rights reserved.
京ICP备2023020795号-1
ghs 京公网安备 11010802042870号
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术官方微信