考虑非牛顿引力的快速转动混合星性质研究

发布时间：2018-05-27 03:31

本文选题：混合星 + 物态方程　；参考：《华南理工大学》2012年硕士论文

【摘要】：物态方程是理论研究中子星结构和性质的重要输入量。将物态方程输入TOV方程，就可以得到中子星的内部结构如密度、压强随半径的变化，及质量和半径等宏观特性。不同的物态方程，会得出迥然不同的中子星宏观特征。中子星的质量和半径是其重要的外部特性，对于基本物理理论的验证有着非常关键的作用。对中子星质量的观测将对中子星的物态方程提供有效的约束，特别是大质量中子星的观测发现。最近观测到的PSRJ1614-2230中子星具有较大的星体质量，被精确测定为1.97±0.04M⊙(其中M⊙为太阳质量：2×10~(30)kg)对中子星物质物态方程提供了较为严格的约束，即在经典理论框架下它将排除所有较软的物态方程。在各种理论模型中，超子态、夸克态等的出现将会使物态方程软化。例如，混合星模型的物态方程就具有较软的物态方程。同时，地面重离子碰撞试验也支持高密度非对称核物质具有较软物态方程的结论。那么，大质量的中子星的发现，，是否真的可以排除较软的物态方程呢？在对引力的认识还并不完善的今天，我们对此并不能给出肯定的答案。早就被试验证实的小尺度下引力将严重偏离牛顿引力的事实提醒我们：在致密天体中这种非牛顿引力可能会具有明显的物理效应。研究表明，非牛顿引力为软物态方程支持大质量中子星提供了一种有效的物理机制。本论文主要研究了考虑非牛顿引力下的快速转动混合星（hybrid star）的结构和性质：包括质量——半径关系、Kepler转速、转动惯量、引力红移以及转动动能和引力结合能之比等。结果表明，非牛顿引力和快速转动都会有效地增大混合星能支持的最大质量；Kepler转速下能支持的最大质量比静态时增加约20%左右。转动对于考虑非牛顿引力的混合星整体结构性质（包括质量——半径关系、转动惯量、转动动能和引力结合能之比等）都具有明显的影响，但对极向引力红移影响相对较小。
[Abstract]:The equation of state is an important input for the theoretical study of the structure and properties of neutron stars. When the equation of state is input into the TOV equation, the internal structure of the neutron star, such as the variation of the density, the pressure with the radius, the mass and the radius, and so on, can be obtained. Different equations of state will result in very different macro characteristics of neutron stars. The mass and radius of neutron stars are important external properties and play a very important role in the verification of basic physical theory. The observation of neutron star mass will provide an effective constraint on the equation of state of neutron star, especially the observation of large mass neutron star. The recently observed PSRJ1614-2230 neutron star has a large stellar mass, which has been accurately determined to be 1.97 卤0.04M _ (?) (where M _ (?) is the solar mass of 2 脳 10 ~ (2) 脳 10 ~ (2) ~ (30) kg), which provides a relatively strict constraint on the equation of state of matter of the neutron star. That is, under the framework of classical theory, it will exclude all the softer equations of state. In various theoretical models, the occurrence of hyperon and quark states will soften the equation of state. For example, the equation of state of the mixed star model has a softer equation of state. At the same time, the ground heavy ion collision test also supports the conclusion that high density asymmetric nuclear matter has a soft equation of state. So can the discovery of a massive neutron star really exclude the softer equation of state? In today's imperfect understanding of gravity, we cannot give a definite answer to it. The fact that gravity will deviate seriously from Newton's gravity on a small scale, which has long been proved by experiments, reminds us that this kind of non-Newtonian gravity may have obvious physical effects in dense celestial bodies. It is shown that non-Newtonian gravitation provides an effective physical mechanism for the support of large mass neutron stars by the equations of state of soft matter. In this paper, the structure and properties of hybrid stars with fast rotation considering non-Newtonian gravity are studied, including the mass-radius relation Kepler rotational speed, moment of inertia, gravitational redshift and the ratio of rotational kinetic energy to gravitational binding energy. The results show that both non-Newtonian gravity and rapid rotation can effectively increase the maximum mass supported by the mixed star at Kepler speed by about 20% compared with the static one. Rotation has obvious influence on the global structure properties of mixed stars considering non-Newtonian gravity (including mass-radius relation, moment of inertia, ratio of rotational kinetic energy to gravitational binding energy, etc.), but has relatively little effect on the red shift of polar gravity.
【学位授予单位】：华南理工大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P145.6

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