$f(\mathcal{G},T)$引力中的恒星流体静力平衡紧致结构
Stellar Hydrostatic Equilibrium Compact Structures in $f(\mathcal{G},T)$ Gravity
摘要：
本文在$f(\mathcal{G},T)$引力模型下研究了致密星（中子星和奇异星）的恒星流体静力平衡位形，其中$\mathcal{G}$和$T$分别是Gauss-Bonnet不变量和能量动量张量的迹。在推导了$f(\mathcal{G},T)$引力的流体静力平衡方程后，利用对应于两个不同致密星的两个状态方程模型，计算了中子星和奇异星的流体压力。对于$f(\mathcal{G},T)=α{\mathcal{G}^n+λ{T}}$重力模型，$α$、$n$和$λ$是一些特定的常数，致密恒星的物理属性如能量密度、压力、恒星质量和总半径的行为发生了实质性的变化，相应的$λ$值也发生了变化。同时，对于一定的中心能量密度，随着$λ$的增大，中子星和奇异星的质量都增大，而两种致密星的总半径$R$则相反.结果表明，对于这种$f(\mathcal{G},T)$恒星模型，最大恒星质量可以被推高到观测极限以上。
英文摘要：
In this paper, stellar hydrostatic equilibrium configuration of the compact stars (neutron stars and strange stars) has been studied for $f(\mathcal{G},T)$ gravity model, with $\mathcal{G}$ and $T$ being the Gauss-Bonnet invariant and the trace of energy momentum tensor, respectively. After having derived the hydrostatic equilibrium equations for $f(\mathcal{G},T)$ gravity, the fluid pressure for the neutron stars and the strange stars has been computed by implying two equation of state models corresponding to two different existing compact stars. For the $f(\mathcal{G},T)=α{\mathcal{G}^n+λ{T}}$ gravity model, with $α$, $n$, and $λ$ being some specific constants, substantial change in the behavior of the physical attributes of the compact stars like the energy density, pressure, stellar mass, and total radius has been noted with the corresponding change in $λ$ values. Meanwhile, it has been shown that for some fixed central energy density and with increasing values of $λ$, the stellar mass both for the neutron stars and the strange stars increases, while the total stellar radius $R$ exhibits the opposite behavior for both of the compact stars. It is concluded that for this $f(\mathcal{G},T)$ stellar model, the maximum stellar mass can be boosted above the observational limits.
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