论文标题
$ f（r，t）$重力中快速旋转的中子星
Rapidly rotating neutron stars in $f(R,T)$ gravity
论文作者
论文摘要
在这项工作中，我们研究了$ f（r，t）$重力对快速旋转中子星的影响。首先，我们讨论这种修改的重力理论的主要方面，其中重力拉格朗日是RICCI标量$ r $的任意函数，以及能量巨头张量$ t $的痕迹。然后，我们介绍了中子恒星的基本方程式，包括目前工作中用于描述辐射物质的状态方程。计算了一些物理量的兴趣，例如质量 - 拉迪乌斯关系，惯性矩，角动量和紧凑性。通过考虑四个不同的旋转状态，我们获得的结果表明与一般相对性的情况相比，与$ f（r，t）$重力相比，中子星的物理特性进行了重大修改。特别是，恒星序列的质量 - 拉迪乌斯关系表明，$ f（r，t）$重力增加了中子星的质量和赤道半径，恒星的恒星旋转，角速度小于开普勒极限。
In this work, we study the influence of $f(R,T)$ gravity on rapidly rotating neutron stars. First we discuss the main aspects of this modified theory of gravity where the gravitational Lagrangian is an arbitrary function of the Ricci scalar $R$ and of the trace of the energy-momentum tensor $T$. Then we present the basic equations for neutron stars including the equations of state used in the present work to describe the hadronic matter. Some physical quantities of interest are calculated such as mass-radius relations, moments of inertia, angular momentum, and compactness. By considering four different rotation regimes, we obtain results that indicate substantial modifications in the physical properties of neutron stars in $f(R,T)$ gravity when compared to those in the context of general relativity. In particular, the mass-radius relation for sequences of stars indicates that $f(R,T)$ gravity increases the mass and the equatorial radius of the neutron stars for stars rotating with an angular velocity smaller than Kepler limit.
