论文标题
$ d \ rightarrow 4 $高斯重力的极限
Anisotropic compact stars in $D\rightarrow 4$ limit of Gauss-Bonnet gravity
论文作者
论文摘要
基于以下事实：使用任何正则化方案得出的球形对称解决方案将与原始理论\ cite \ cite {Banerjee：2020yhu，Hennigar，Hennigar：2020LSL，Casalino，Casalino：202020kbt，aoki：202020 ligrigrighation atery Interrigy atery Interrighation：假设具有两个常数的度量电位的特定形式。使用结条件，我们确定这两个常数。 By using the data of the star EXO $1785-248 $, whose mass is $ { M=1.3\pm0.2 \,{\textrm M}_\odot}$ and radius $ { l=8.849\pm0.4\,{\textrm km}}$, we calculate the numerical values of these constants, in terms of the dimensionful coupling parameter在高斯 - 骨网术语中，最终，我们获得了这些常数的实际价值。在这方面，我们表明能量量张量的组件在恒星的中心具有有限的值，以及恒星表面的较小值。此外，我们表明，由于高斯词的影响，国家方程式以非线性方式行事。使用Tolman-Oppenheimer-Volkoff方程，绝热指数和静态状态的稳定性，我们表明所考虑的模型始终是稳定的。最后，这项研究的解决方案与其他脉冲星的观察数据匹配，显示出令人满意的结果
In the frame of Gauss-Bonnet gravity and in the limit of $D\to 4$, based on the fact that spherically symmetric solution derived using any of regularization schemes will be the same form as the original theory \cite{Banerjee:2020yhu,Hennigar:2020lsl,Casalino:2020kbt,Aoki:2020lig}, we derive a new interior spherically symmetric solution assuming specific forms of the metric potentials that have two constants . Using the junction condition we determine these two constants. By using the data of the star EXO $1785-248 $, whose mass is $ { M=1.3\pm0.2 \,{\textrm M}_\odot}$ and radius $ { l=8.849\pm0.4\,{\textrm km}}$, we calculate the numerical values of these constants, in terms of the dimensionful coupling parameter of the Gauss-Bonnet term, and eventually, we get real values for these constants. In this regard, we show that the components of the energy-momentum tensor has a finite value at the center of the star as well as a smaller value to the surface of the star. Moreover, we show that the equations of the state behave in a non-linear way due to the impact of the Gauss-Bonnet term. Using the Tolman-Oppenheimer-Volkoff equation, the adiabatic index, and stability in the static state we show that the model under consideration is always stable. Finally, the solution of this study is matched with observational data of other pulsars showing satisfactory results
