费米子暗物质对中子星结构和冷却性质的影响
发布时间：2018-08-20 08:42
【摘要】：中子星是大质量恒星在演化的晚期、超新星爆发之后,在其中心形成的致密星体,是目前所能观测到的高温高密星体之一。鉴于其宏观性质的可观测性,中子星为人们提供了一个研究致密物质的天然实验室。但是,由于人们对高密物质认识的匮乏,对中子星的描述还有许多不确定的因素,如:中子星的组成、结构、冷却性质等。暗物质可能是中子星的组成成分,且它对中子星的结构、演化、热辐射、磁场、以及观测都有重大影响。目前,多数学者都侧重于研究暗物质对中子星结构的影响,本文在前人研究的基础上,继续探索暗物质对中子星冷却性质的影响。本文分成四个部分:第一部分是关于暗物质的历史回顾和研究现状,介绍暗物质的形成过程、分类、性质和几种简单的暗物质模型。第二部分详细介绍中子星形成的过程、中子星结构,并给出本文的基础理论,包括相对论平均场理论(RMFT)、TOV方程、冷却理论等。第三部分考虑含有暗物质的中子星模型(DANS),采用相对论平均场理论,分别研究暗物质自相互作用为弱作用和强作用两种情况下,费米子暗物质对中子星物态方程(Eo S)和质量—半径关系的影响。第四部分研究不同的暗物质自相互作用、不同的暗物质粒子质量下费米子暗物质对中子星的中微子发射率、中微子发光度和冷却曲线的影响。论文的最后给出结论和展望。
[Abstract]:Neutron stars are dense stars formed in the center of massive stars in the late stage of evolution and after supernova erupts. It is one of the high temperature and high density stars that can be observed at present. Due to its observability, neutron stars provide a natural laboratory for the study of dense matter. However, due to the lack of understanding of high-density matter, there are still many uncertain factors in the description of neutron stars, such as the composition, structure and cooling properties of neutron stars. Dark matter may be a component of a neutron star, and it has a significant impact on the structure, evolution, thermal radiation, magnetic field, and observations of the neutron star. At present, most scholars have focused on the influence of dark matter on the structure of neutron stars. Based on the previous studies, this paper continues to explore the influence of dark matter on the cooling properties of neutron stars. This paper is divided into four parts: the first part is a review of the history of dark matter and the status quo of research, the formation of dark matter, classification, properties and several simple dark matter models. In the second part, the formation process and the structure of neutron star are introduced in detail, and the basic theory of this paper is given, including the relativistic mean field theory (RMFT) 's equation, cooling theory and so on. In the third part, the neutron star model (DANS), with dark matter is considered, and the relativistic mean field theory is used to study the self-interaction of dark matter in the case of weak interaction and strong interaction, respectively. The effect of fermion dark matter on the equation of state (Eo S) and mass-radius relation of neutron stars. In the fourth part, we study the effects of fermion dark matter on neutrino emissivity, neutrino luminosity and cooling curve of neutron stars under different self-interaction of dark matter particles and different mass of dark matter particles. Finally, the conclusion and prospect are given.
【学位授予单位】：渤海大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P145.9;P145.6
[Abstract]:Neutron stars are dense stars formed in the center of massive stars in the late stage of evolution and after supernova erupts. It is one of the high temperature and high density stars that can be observed at present. Due to its observability, neutron stars provide a natural laboratory for the study of dense matter. However, due to the lack of understanding of high-density matter, there are still many uncertain factors in the description of neutron stars, such as the composition, structure and cooling properties of neutron stars. Dark matter may be a component of a neutron star, and it has a significant impact on the structure, evolution, thermal radiation, magnetic field, and observations of the neutron star. At present, most scholars have focused on the influence of dark matter on the structure of neutron stars. Based on the previous studies, this paper continues to explore the influence of dark matter on the cooling properties of neutron stars. This paper is divided into four parts: the first part is a review of the history of dark matter and the status quo of research, the formation of dark matter, classification, properties and several simple dark matter models. In the second part, the formation process and the structure of neutron star are introduced in detail, and the basic theory of this paper is given, including the relativistic mean field theory (RMFT) 's equation, cooling theory and so on. In the third part, the neutron star model (DANS), with dark matter is considered, and the relativistic mean field theory is used to study the self-interaction of dark matter in the case of weak interaction and strong interaction, respectively. The effect of fermion dark matter on the equation of state (Eo S) and mass-radius relation of neutron stars. In the fourth part, we study the effects of fermion dark matter on neutrino emissivity, neutrino luminosity and cooling curve of neutron stars under different self-interaction of dark matter particles and different mass of dark matter particles. Finally, the conclusion and prospect are given.
【学位授予单位】：渤海大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P145.9;P145.6
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