论文标题
在非微小几何耦合理论中，带有2.6 $ m_ \ odot $的夸克之星，重力理论
Quark stars with 2.6 $M_\odot$ in a non-minimal geometry-matter coupling theory of gravity
论文作者
论文摘要
这项工作分析了非最小的几何耦合（GMC）重力理论中奇怪恒星的静水平衡构型。这些恒星是由奇怪的夸克物质制成的，其分布受到麻省理工学院方程的约束。非最小GMC理论通过以下重力动作描述：$ f（r，l）= r/2+l+σrl$，其中$ r $代表曲率标量，$ l $是物质lagrangian密度，$σ$是耦合参数。在考虑这一理论时，奇怪的恒星变得更大，更大。特别是，当$σ= 50 $ km $^2 $时，该理论可以实现2.6 $ m_ \ odot $，这适用于描述PULSARS PSR PSR J2215+5135和PSR J1614-2230，以及GW190814活动中二级对象的质量。 2.6 $ m_ \ odot $即使考虑快速旋转效果也是一般相对论几乎无法实现的，并且与PSR J0952-0607（$ M = 2.35 \ pm 0.17〜m_ \ odot $）的质量兼容，最近在奇特的脉动中，它的分布是奇特的，它的分量是奇特的，它的分量很奇怪。非最小的GMC理论还可以给出可行的结果，以描述奇怪的恒星候选者的宏观特征。
This work analyses the hydrostatic equilibrium configurations of strange stars in a non-minimal geometry-matter coupling (GMC) theory of gravity. Those stars are made of strange quark matter, whose distribution is governed by the MIT equation of state. The non-minimal GMC theory is described by the following gravitational action: $f(R,L)=R/2+L+σRL$, where $R$ represents the curvature scalar, $L$ is the matter Lagrangian density, and $σ$ is the coupling parameter. When considering this theory, the strange stars become larger and more massive. In particular, when $σ=50$ km$^2$, the theory can achieve the 2.6 $M_\odot$, which is suitable for describing the pulsars PSR J2215+5135 and PSR J1614-2230, and the mass of the secondary object in the GW190814 event. The 2.6 $M_\odot$ is a value hardly achievable in General Relativity even considering fast rotation effects, and is also compatible with the mass of PSR J0952-0607 ($M = 2.35 \pm 0.17 ~M_\odot$), the heaviest and fastest pulsar in the disk of the Milky Way, recently measured, supporting the possible existence of strange quark matter in its composition. The non-minimal GMC theory can also give feasible results to describe the macroscopical features of strange star candidates.
