【摘要】：中子星是大質(zhì)量恒星在演化的晚期、超新星爆發(fā)之后,在其中心形成的致密星體,是目前所能觀測到的高溫高密星體之一。鑒于其宏觀性質(zhì)的可觀測性,中子星為人們提供了一個研究致密物質(zhì)的天然實驗室。但是,由于人們對高密物質(zhì)認(rèn)識的匱乏,對中子星的描述還有許多不確定的因素,如:中子星的組成、結(jié)構(gòu)、冷卻性質(zhì)等。暗物質(zhì)可能是中子星的組成成分,且它對中子星的結(jié)構(gòu)、演化、熱輻射、磁場、以及觀測都有重大影響。目前,多數(shù)學(xué)者都側(cè)重于研究暗物質(zhì)對中子星結(jié)構(gòu)的影響,本文在前人研究的基礎(chǔ)上,繼續(xù)探索暗物質(zhì)對中子星冷卻性質(zhì)的影響。本文分成四個部分:第一部分是關(guān)于暗物質(zhì)的歷史回顧和研究現(xiàn)狀,介紹暗物質(zhì)的形成過程、分類、性質(zhì)和幾種簡單的暗物質(zhì)模型。第二部分詳細(xì)介紹中子星形成的過程、中子星結(jié)構(gòu),并給出本文的基礎(chǔ)理論,包括相對論平均場理論(RMFT)、TOV方程、冷卻理論等。第三部分考慮含有暗物質(zhì)的中子星模型(DANS),采用相對論平均場理論,分別研究暗物質(zhì)自相互作用為弱作用和強作用兩種情況下,費米子暗物質(zhì)對中子星物態(tài)方程(Eo S)和質(zhì)量—半徑關(guān)系的影響。第四部分研究不同的暗物質(zhì)自相互作用、不同的暗物質(zhì)粒子質(zhì)量下費米子暗物質(zhì)對中子星的中微子發(fā)射率、中微子發(fā)光度和冷卻曲線的影響。論文的最后給出結(jié)論和展望。
[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.
【學(xué)位授予單位】：渤海大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P145.9;P145.6

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