發(fā)布時(shí)間：2018-10-17 14:39

【摘要】：本文對(duì)中子星的形成過程、觀測(cè)機(jī)制、組成成分、發(fā)展歷史和研究意義進(jìn)行了詳細(xì)的描述，對(duì)中子星研究的發(fā)展歷程和現(xiàn)取得的成果進(jìn)行了歸納總結(jié)。以這些研究成果為基礎(chǔ)，本文主要開展了兩部分研究。 第一部分，在多體理論和量子場(chǎng)理論的框架下，利用相對(duì)論介子模型的平均場(chǎng)近似，，探討中子星殼層物質(zhì)的核對(duì)稱能與不可壓縮系數(shù)的關(guān)系。研究結(jié)果表明，在不同的耦合常數(shù)情況下，對(duì)稱能都隨著重子數(shù)密度的增大而增大。在固定自耦合常數(shù)d時(shí)對(duì)稱能隨著飽和密度下的不可壓縮系數(shù)增大而增加。而固定自耦合常數(shù)c時(shí)對(duì)稱能則隨著飽和密度下的不可壓縮系數(shù)增大而減小。分別固定耦合常數(shù)g v和g s時(shí)，對(duì)稱能隨著飽和密度下的不可壓縮系數(shù)的改變基本沒有變化。這表明，核子間的耦合常數(shù)對(duì)核對(duì)稱能的影響比自耦合常數(shù)大。 第二部分，引入自洽的邊界條件求解了非均勻介子場(chǎng)方程，并采用Thomas-Fermi近似來描述中子星殼層物質(zhì)的物態(tài)方程。研究結(jié)果表明,中子星殼層物質(zhì)的平均能量密度和壓強(qiáng)隨著核子數(shù)密度的增大而變大，粒子數(shù)密度和核子能量密度從晶胞中心開始減小。當(dāng)粒子數(shù)密度n B增大時(shí)，晶胞的半徑減小，當(dāng)粒子數(shù)密度nB0.06fm3時(shí)，核子已經(jīng)瓦解不復(fù)存在。以上結(jié)果與現(xiàn)有研究成果非常吻合，說明引入自洽的模型研究中子星殼層物質(zhì)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.
【學(xué)位授予單位】：暨南大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2013
【分類號(hào)】：P145.6

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 章利良,宋宏秋;FST模型中核物質(zhì)的不可壓縮系數(shù)[J];高能物理與核物理;2000年03期

本文編號(hào)：2277003