本文選題：中子星 + U玻色子　； 參考：《渤海大學(xué)》2015年碩士論文

【摘要】：中子星以高溫高密度著稱,是20世紀(jì)六十年代天文學(xué)的四大發(fā)現(xiàn)之一。對中子星的研究有利于人們認(rèn)識致密物質(zhì)、發(fā)現(xiàn)致密物質(zhì)間的相互作用規(guī)律,甚至發(fā)現(xiàn)新的物質(zhì)形態(tài)。然而幾十年過去了,對中子星的研究仍然沒有取得突破性進(jìn)展,中子星的物質(zhì)組成、結(jié)構(gòu)、冷卻性質(zhì)等還存在著很多不確定因素。隨著天文觀測水平的進(jìn)步,引力修正理論正逐漸獲得人們的認(rèn)可和關(guān)注,在中子星這樣的高密度下,考慮引力修正是必要且重要的,因此本文著重研究引力修正對中子星結(jié)構(gòu)和冷卻性質(zhì)的影響。本論文采用相對論平均場理論(RMFT)和弱作用冷卻理論來研究中子星的結(jié)構(gòu)和星體冷卻性質(zhì)�？紤]引力修正效應(yīng),在上述理論中引入U玻色子。討論的中子星物質(zhì)包括兩種,一種是正常中子星物質(zhì)(包括質(zhì)子、中子、電子和m子),另一種是進(jìn)一步包含-D和0D的中子星物質(zhì)(包括質(zhì)子、中子、電子、m子、-D和0D,簡稱0DD-np物質(zhì))。全文共分五部分,第一部分是中子星觀測方面的概述,介紹中子星質(zhì)量、表面引力紅移和旋轉(zhuǎn)方面的觀測進(jìn)展;第二部分詳細(xì)給出研究所用的理論,包括相對論平均場理論、Tolman-Oppenheimer-Volkoff(TOV)方程、弱作用冷卻理論等;第三部分研究U玻色子對中子星結(jié)構(gòu)的影響,探索不同的U玻色子耦合強(qiáng)度與中子星的物態(tài)方程(EoS)、質(zhì)量和半徑等的關(guān)系;第四部分研究不同的U玻色子耦合強(qiáng)度對中子星的中微子發(fā)射率的影響,給出中子星內(nèi)部核子直接URCA(dURCA)過程發(fā)生的范圍;第五部分主要探討引力修正對中子星冷卻性質(zhì)的影響,研究中子星的中微子發(fā)光度、冷卻曲線等在引力修正效應(yīng)下的行為。論文的最后給出結(jié)論和展望。
[Abstract]:Neutron stars, known for their high temperature and density, were one of the four discoveries of astronomy in the 1960 s. The study of neutron stars is beneficial to the understanding of dense matter, the law of interaction between dense matter, and even the discovery of new material forms. However, after several decades, there is still no breakthrough in the study of neutron stars, and there are still many uncertain factors in the composition, structure and cooling properties of neutron stars. With the progress of astronomical observation, the theory of gravity correction is gradually gaining recognition and attention. It is necessary and important to consider gravitational correction under the high density of neutron star. Therefore, the influence of gravity correction on the structure and cooling properties of neutron stars is studied in this paper. In this paper, the relativistic mean field theory (RMFT) and the weak interaction cooling theory are used to study the structure and cooling properties of neutron stars. Considering the gravitational correction effect, the U boson is introduced in the above theory. The neutron star matter discussed consists of two types, one is normal neutron star matter (including protons, neutrons, electrons and mons), the other is neutron star matter (including protons, neutrons, electrons, and neutrons) that further contains -D and 0D. The electron meconium D and 0D, referred to as 0DD-np substance. The paper is divided into five parts. The first part is an overview of neutron star observation, which introduces the observation progress of neutron star mass, surface gravity redshift and rotation. The relativistic mean field theory includes Tolman-Oppenheimer-Volkofftov equation, weak interaction cooling theory, etc. In the third part, the influence of U boson on neutron star structure is studied, and the relationship between the coupling strength of U boson and the equation of state, mass and radius of neutron star is discussed. In the fourth part, we study the influence of different U boson coupling strength on the neutrino emissivity of neutron star, and give the range of the nuclear direct URCAD Urca process in neutron star, the fifth part mainly discusses the influence of gravity correction on the cooling property of neutron star. The behavior of neutrino luminosity and cooling curve of neutron stars under gravitational correction effect is studied. 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】：2015
【分類號】：P145.6

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 文德華;荊珍珍;;軟物態(tài)方程支持大質(zhì)量中子星機(jī)制概述[J];原子核物理評論;2014年03期

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本文編號：1950706