中子星壳层与对称能
发布时间：2018-10-17 14:39
【摘要】：本文对中子星的形成过程、观测机制、组成成分、发展历史和研究意义进行了详细的描述，对中子星研究的发展历程和现取得的成果进行了归纳总结。以这些研究成果为基础，本文主要开展了两部分研究。 第一部分，在多体理论和量子场理论的框架下，利用相对论介子模型的平均场近似，，探讨中子星壳层物质的核对称能与不可压缩系数的关系。研究结果表明，在不同的耦合常数情况下，对称能都随着重子数密度的增大而增大。在固定自耦合常数d时对称能随着饱和密度下的不可压缩系数增大而增加。而固定自耦合常数c时对称能则随着饱和密度下的不可压缩系数增大而减小。分别固定耦合常数g v和g s时，对称能随着饱和密度下的不可压缩系数的改变基本没有变化。这表明，核子间的耦合常数对核对称能的影响比自耦合常数大。 第二部分，引入自洽的边界条件求解了非均匀介子场方程，并采用Thomas-Fermi近似来描述中子星壳层物质的物态方程。研究结果表明,中子星壳层物质的平均能量密度和压强随着核子数密度的增大而变大，粒子数密度和核子能量密度从晶胞中心开始减小。当粒子数密度n B增大时，晶胞的半径减小，当粒子数密度nB0.06fm3时，核子已经瓦解不复存在。以上结果与现有研究成果非常吻合，说明引入自洽的模型研究中子星壳层物质非常成功。
[Abstract]:In this paper, the formation process, observation mechanism, composition, development history and research significance of neutron star are described in detail, and the development course and achievements of neutron star research are summarized. Based on these research results, this paper mainly carried out two parts of research. In the first part, under the framework of multi-body theory and quantum field theory, using the mean field approximation of relativistic meson model, the relationship between the nuclear symmetry energy of neutron star shell and the incompressible coefficient is discussed. The results show that the symmetry energy increases with the increase of baryon number density under different coupling constants. When the self-coupling constant d is fixed, the symmetric energy increases with the increase of the incompressible coefficient at saturation density. When the self-coupling constant c is fixed, the symmetric energy decreases with the increase of the incompressible coefficient at saturation density. When the coupling constants g v and g s are fixed respectively, the symmetry energy is basically unchanged with the change of the incompressibility coefficient at saturation density. It is shown that the effect of the coupling constant between nucleons on the nuclear symmetry energy is greater than that on the self-coupling constant. In the second part, the self-consistent boundary condition is introduced to solve the nonuniform meson field equation, and the Thomas-Fermi approximation is used to describe the equation of state of the neutron star shell. The results show that the average energy density and pressure of the neutron star shell increase with the increase of the nucleon number density, and the particle number density and the nuclear energy density begin to decrease from the center of the cell. When the density of particle number NB increases, the radius of unit cell decreases, and when the density of particle number is nB0.06fm3, the nucleon disintegrates and no longer exists. The above results are in good agreement with the existing research results, which indicates that the self-consistent model is very successful in the study of neutron star shell matter.
【学位授予单位】：暨南大学
【学位级别】：硕士
【学位授予年份】：2013
【分类号】：P145.6
本文编号：2277003
[Abstract]:In this paper, the formation process, observation mechanism, composition, development history and research significance of neutron star are described in detail, and the development course and achievements of neutron star research are summarized. Based on these research results, this paper mainly carried out two parts of research. In the first part, under the framework of multi-body theory and quantum field theory, using the mean field approximation of relativistic meson model, the relationship between the nuclear symmetry energy of neutron star shell and the incompressible coefficient is discussed. The results show that the symmetry energy increases with the increase of baryon number density under different coupling constants. When the self-coupling constant d is fixed, the symmetric energy increases with the increase of the incompressible coefficient at saturation density. When the self-coupling constant c is fixed, the symmetric energy decreases with the increase of the incompressible coefficient at saturation density. When the coupling constants g v and g s are fixed respectively, the symmetry energy is basically unchanged with the change of the incompressibility coefficient at saturation density. It is shown that the effect of the coupling constant between nucleons on the nuclear symmetry energy is greater than that on the self-coupling constant. In the second part, the self-consistent boundary condition is introduced to solve the nonuniform meson field equation, and the Thomas-Fermi approximation is used to describe the equation of state of the neutron star shell. The results show that the average energy density and pressure of the neutron star shell increase with the increase of the nucleon number density, and the particle number density and the nuclear energy density begin to decrease from the center of the cell. When the density of particle number NB increases, the radius of unit cell decreases, and when the density of particle number is nB0.06fm3, the nucleon disintegrates and no longer exists. The above results are in good agreement with the existing research results, which indicates that the self-consistent model is very successful in the study of neutron star shell matter.
【学位授予单位】：暨南大学
【学位级别】：硕士
【学位授予年份】：2013
【分类号】：P145.6
【参考文献】
相关期刊论文 前1条
1 章利良,宋宏秋;FST模型中核物质的不可压缩系数[J];高能物理与核物理;2000年03期
本文编号：2277003
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