arXiv 2107.016452021-07gr-qc

远平行引力下中子星的恒星解析模型

Analytical Stellar Models of Neutron Stars in Teleparallel Gravity

Jay Solanki, Rohan Joshi, Malay Garg

备注：: made equations more readable and implemented some changes suggested by reviewers
DOI：: 10.1007/s12648-022-02446-5

摘要：

在本文中，我们发展了三个分析模型，并得到了一类新的解决方案，描述紧凑的恒星结构的远平行引力理论。我们考虑一般的各向异性性质的恒星配置和解决远程平行引力方程。为了深入分析恒星的各种参数，我们通过选择各种物理上可接受的度量势$ e^{d(r)} $和径向压力$ p_r(r) $的形式，建立了三个模型。我们还分析了遥平行引力参数$ β$和$ β_1 $对恒星结构描述的影响。我们计算了模型参数，使得描述各种观测到的中子星的模型遵守所有的物理条件，成为潜在稳定和因果关系。通过分析远平行引力场的各种参数对描述各向异性恒星结构的影响，发现本文建立的三种模型可以描述从低密度到高密度的各向异性中子星。最后，我们得到了描述不同中子星模型的二次状态方程，它可以用来寻找恒星结构的组成。由于许多学者发现真实中子星和奇异星的物质组成具有二次物态方程，因此寻找具有二次物态方程的模型是非常有用的。非线性$ f(T) $模型给出的物态方程与二次行为的偏差较大，因此，本文采用线性$ f(T) $函数，利用对角四元体来模拟致密星。

英文摘要：

In this paper, we developed three analytical models and obtained a new class of solutions describing compact stellar structures using the theory of teleparallel gravity. We consider the general anisotropic nature of stellar configurations and solve teleparallel gravity equations. In order to thoroughly analyze the various parameters of the stars, we developed three models by choosing various physically acceptable forms of metric potential $ e^{d(r)} $ and radial pressure $ p_r(r) $. We also analyze the impact of teleparallel gravity's parameters $ β$ and $ β_1 $ on the description of the stellar structures. We calculated model parameters such that models describing various observed neutron stars obey all physical conditions to be potentially stable and causal. By analyzing the impact of various parameters of teleparallel gravity on the description of anisotropic stellar structures, we found that three models developed in this paper can describe anisotropic neutron stars ranging from low density to high density. Finally, we obtain a quadratic Equation of State for each model describing various neutron stars, which can be utilized to find compositions of the stellar structures. It is very useful to find models that can exhibit quadratic EOS, since material compositions of real neutron stars and strange stars are found to exhibit quadratic EOS by various authors. Non linear $ f(T) $ model gives high deviation of EOS from quadratic behaviour, thus, in this paper we work with linear $ f(T) $ function by using diagonal tetrad to model realistic compact stars.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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英文摘要：

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