Δ共振态存在于中子星内部可能性的探讨

发布时间：2018-09-12 12:43

【摘要】：中子星作为致密物质的天然实验室，一直是很多学者研究的热门课题。本文一方面采用相对论平均场理论来研究Δ共振态在不同中子星物质（传统中子星物质、超子物质、K介子凝聚等）中的性质，研究Δ共振态对中子星粒子分布、质量-半径关系等方面性质的影响，进而证明Δ共振态可以存在于中子星的内部。另一方面，以弱相互作用理论为基础，研究Δ共振态对核子的直接URCA过程及中子星冷却过程的影响。最后，以脉冲星J1614-2230为例，研究Δ共振态对它的影响。结果表明，脉冲星J1614-2230的内核可以由传统中子星物质和Δ共振态构成，并且Δ~（-）和Δ~（0）粒子所占的比例可高达百分之三十。Δ共振态对冷却的影响较为复杂，它们能够降低中微子的发射率和发光度，但是在传统中子星物质中，Δ共振态加速中子星冷却。本文的主要内容如下：第一章回顾中子星研究的发展历史，介绍中子星的性质，以及目前国内外对中子星的研究现状，并提出对未来的展望。第二章介绍基本的研究理论，，分析Δ共振态存在于传统中子星物质及超子物质中的可能性，研究在这两种物质中Δ共振态对中子星微观及宏观性质的影响。第三章给出Δ共振态可以出现在含反K介子凝聚中子星内部的依据。分析Δ共振态与反K介子互相影响的性质，并研究它们对中子星的影响。第四章介绍中子星的冷却理论，并且讨论Δ共振态对核子的直接URCA过程、中微子发射率、中微子发光度、冷却曲线等方面的影响。第五章研究Δ共振态存在于具体的中子星内部的情况（比如脉冲星J1614-2230），给出他们存在的径向范围、粒子数所占比例、冷却等性质。
[Abstract]:As a natural laboratory of dense matter, neutron star has been a hot topic for many scholars. On the one hand, the relativistic mean field theory is used to study the properties of 螖 resonance state in different neutron star matter (traditional neutron star matter, hyperon matter K meson condensation, etc.) and the distribution of 螖 resonance state to neutron star particle. It is proved that the 螖 resonance state can exist inside the neutron star due to the influence of the mass-radius relation. On the other hand, based on the weak interaction theory, the influence of 螖 resonance state on the direct URCA process of nucleon and the cooling process of neutron star is studied. Finally, the effect of 螖 resonance on the pulsar J1614-2230 is studied. The results show that the core of pulsar J1614-2230 can be composed of conventional neutron star matter and 螖 resonance state, and the proportion of 螖 ~ (-) and 螖 ~ (0) particles can be as high as 30%. The effect of 螖 resonance state on cooling is more complex. They can reduce the emissivity and luminosity of neutrino, but in conventional neutron star matter, 螖 resonance state accelerates the cooling of neutron star. The main contents of this paper are as follows: the first chapter reviews the development history of neutron star research, introduces the nature of neutron star, and the present research status of neutron star at home and abroad, and puts forward the prospect for the future. The second chapter introduces the basic research theory, analyzes the possibility of 螖 resonance state in the traditional neutron star matter and hyperon matter, and studies the influence of 螖 resonance state on the microscopic and macroscopic properties of neutron star in these two kinds of matter. In chapter 3, we give the basis for 螖 resonance state to appear in the neutron star with inverse K meson condensation. The properties of the interaction between 螖 resonance states and inverse K mesons are analyzed and their effects on neutron stars are studied. In chapter 4, the cooling theory of neutron star is introduced, and the effects of 螖 resonance state on the direct URCA process, neutrino emissivity, neutrino luminosity and cooling curve are discussed. In chapter 5, we study the existence of 螖 resonance in the interior of a specific neutron star (for example, pulsar J1614-2230), and give their radial range, the proportion of particles, cooling and so on.
【学位授予单位】：渤海大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P145.6

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