致密星非径向振动的研究
发布时间：2018-10-18 07:28
【摘要】：首先，我们阐述了中子星结构和性质的研究现状及意义，以及致密星非径向振动f-mode的研究方法。在后面的两个主要部分，计算并讨论了中子星和夸克星的f-mode振动频率和衰减时间。 详细地，我们利用普遍用来计算致密星结构的广义相对论下球对称理想流体静力学平衡方程(TOV方程)，并且饱和核密度附近给定对称能斜率一个合理的范围，计算了中子星的质量-半径关系，以及中子星非径向振动f-mode的振动频率和衰减时间，同时获得了频率和衰减时间的约束范围。结果表明：较大的对称能斜率对应着较小的振动频率和较长的衰减时间；与牛顿理论做对比，广义相对论下计算出的f-mode振动频率跟平均密度的平方根存在类似的比例关系；并且以致密度(M R)作为自变量，以含有衰减时间的函数作为因变量进行合理的拟合。 另一方面，非牛顿引力的提出是为了使地面实验给出的软物态可以支持观测到的大质量脉冲星，它提供一种排斥力，在物理上类似于暗能量的作用。本文在夸克星内考虑了非牛顿引力，，夸克星物质的状态方程用MIT口袋模型来描述，同样计算了夸克星的质量-半径关系和f-mode的振动频率和衰减时间。研究发现：对较大的口袋参数B，即B=117MeVfm-3时，计算出的夸克星最大质量为观测到的典型脉冲星的质量，非牛顿引力应该被考虑。而且我们的计算结果显示，与传统的中子星相比，星体质量相同时夸克星拥有相对较高的f-mode振动频率。
[Abstract]:Firstly, we describe the present situation and significance of the study on the structure and properties of neutron stars, as well as the research methods of nonradial vibration f-mode for dense stars. The f-mode vibration frequency and attenuation time of neutron star and quark star are calculated and discussed in the following two main parts. In detail, we use the spherical symmetric ideal hydrostatic equilibrium equation (TOV equation), which is generally used to calculate compact star structures, and give a reasonable range of symmetric energy slope near the density of saturated nuclei. The mass-radius relation of the neutron star, the vibration frequency and attenuation time of the non-radial vibration f-mode of the neutron star are calculated, and the constraint range of the frequency and attenuation time is obtained. The results show that the larger symmetric energy slope corresponds to smaller vibration frequency and longer attenuation time, and compared with Newton's theory, the f-mode vibration frequency calculated under general relativity has a similar proportional relationship with the square root of average density. The density (M R) is regarded as the independent variable and the function with attenuation time as the dependent variable. On the other hand, the non-Newtonian gravity is proposed to support the observed large mass pulsars in the soft state given by the ground experiments, which provides a repulsive force that is physically similar to the action of dark energy. In this paper, non-Newtonian gravity is considered in quark stars. The equation of state of quark stars is described by MIT pocket model. The mass-radius relation of quark stars and the vibration frequency and attenuation time of f-mode are also calculated. It is found that the calculated maximum mass of the quark star is the mass of the observed typical pulsar for the larger pocket parameter B, that is, B=117MeVfm-3, and the non-Newtonian gravity should be taken into account. Furthermore, our results show that quark stars have relatively high f-mode vibration frequency when the mass of the stars is the same as that of the conventional neutron stars.
【学位授予单位】：华南理工大学
【学位级别】：硕士
【学位授予年份】：2014
【分类号】：P145.6
本文编号：2278419
[Abstract]:Firstly, we describe the present situation and significance of the study on the structure and properties of neutron stars, as well as the research methods of nonradial vibration f-mode for dense stars. The f-mode vibration frequency and attenuation time of neutron star and quark star are calculated and discussed in the following two main parts. In detail, we use the spherical symmetric ideal hydrostatic equilibrium equation (TOV equation), which is generally used to calculate compact star structures, and give a reasonable range of symmetric energy slope near the density of saturated nuclei. The mass-radius relation of the neutron star, the vibration frequency and attenuation time of the non-radial vibration f-mode of the neutron star are calculated, and the constraint range of the frequency and attenuation time is obtained. The results show that the larger symmetric energy slope corresponds to smaller vibration frequency and longer attenuation time, and compared with Newton's theory, the f-mode vibration frequency calculated under general relativity has a similar proportional relationship with the square root of average density. The density (M R) is regarded as the independent variable and the function with attenuation time as the dependent variable. On the other hand, the non-Newtonian gravity is proposed to support the observed large mass pulsars in the soft state given by the ground experiments, which provides a repulsive force that is physically similar to the action of dark energy. In this paper, non-Newtonian gravity is considered in quark stars. The equation of state of quark stars is described by MIT pocket model. The mass-radius relation of quark stars and the vibration frequency and attenuation time of f-mode are also calculated. It is found that the calculated maximum mass of the quark star is the mass of the observed typical pulsar for the larger pocket parameter B, that is, B=117MeVfm-3, and the non-Newtonian gravity should be taken into account. Furthermore, our results show that quark stars have relatively high f-mode vibration frequency when the mass of the stars is the same as that of the conventional neutron stars.
【学位授予单位】：华南理工大学
【学位级别】：硕士
【学位授予年份】：2014
【分类号】：P145.6
【参考文献】
相关期刊论文 前3条
1 燕晶;文得华;;R-mode Instability of Neutron Star with Non-Newtonian Gravity[J];Communications in Theoretical Physics;2013年01期
2 文德华;周颖;;Effects of the symmetry energy slope on the axial oscillations of neutron stars[J];Chinese Physics B;2013年08期
3 文德华;付宏洋;陈伟;;Impact of neutron star crust on gravitational waves from the axial w-modes[J];Chinese Physics B;2011年06期
本文编号：2278419
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