考虑引力修正效应的大质量中子星冷却性质研究

发布时间：2018-05-29 11:24

本文选题：中子星 + U玻色子　；参考：《渤海大学》2015年硕士论文

【摘要】：中子星以高温高密度著称,是20世纪六十年代天文学的四大发现之一。对中子星的研究有利于人们认识致密物质、发现致密物质间的相互作用规律,甚至发现新的物质形态。然而几十年过去了,对中子星的研究仍然没有取得突破性进展,中子星的物质组成、结构、冷却性质等还存在着很多不确定因素。随着天文观测水平的进步,引力修正理论正逐渐获得人们的认可和关注,在中子星这样的高密度下,考虑引力修正是必要且重要的,因此本文着重研究引力修正对中子星结构和冷却性质的影响。本论文采用相对论平均场理论(RMFT)和弱作用冷却理论来研究中子星的结构和星体冷却性质。考虑引力修正效应,在上述理论中引入U玻色子。讨论的中子星物质包括两种,一种是正常中子星物质(包括质子、中子、电子和m子),另一种是进一步包含-D和0D的中子星物质(包括质子、中子、电子、m子、-D和0D,简称0DD-np物质)。全文共分五部分,第一部分是中子星观测方面的概述,介绍中子星质量、表面引力红移和旋转方面的观测进展;第二部分详细给出研究所用的理论,包括相对论平均场理论、Tolman-Oppenheimer-Volkoff(TOV)方程、弱作用冷却理论等;第三部分研究U玻色子对中子星结构的影响,探索不同的U玻色子耦合强度与中子星的物态方程(EoS)、质量和半径等的关系;第四部分研究不同的U玻色子耦合强度对中子星的中微子发射率的影响,给出中子星内部核子直接URCA(dURCA)过程发生的范围;第五部分主要探讨引力修正对中子星冷却性质的影响,研究中子星的中微子发光度、冷却曲线等在引力修正效应下的行为。论文的最后给出结论和展望。
[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.
【学位授予单位】：渤海大学
【学位级别】：硕士
【学位授予年份】：2015
【分类号】：P145.6

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