In this study, our main focus is to investigate the mass–radius relation and several important properties of massive neutron stars to realize the nature, behavior and evolution of these kinds of compact objects at present time. Also, we want to understand the equation-of-state of the core nuclear matter precisely with their stable equilibrium configuration. We have chosen a few massive binary pulsars and investigated on maximum attainable mass and lowest possible radius of them. We have considered Einstein–Hilbert action as $f(R,T)=R+\alpha T$, where $R$ is the Ricci scalar and $T$, the trace of energy–momentum tensor with $\alpha$ as the coupling parameter and also used modified TOV equations. The interior space-time of the spherical neutron star is matched to the exterior Schwarzschild line element at the surface of the star. The $M$–$R$ curve can predict the maximum achievable mass is about $3.51M_{\odot }$ with lowest possible radius of around $10.5$ km for the massive compact stars under stable equilibrium. We have obtained a clear picture of structural evolution of massive neutron stars through accelerating space-time and can put some constraints on several quantities related to them. It is depicted from our present investigation that all the derived outcomes are compatible with physically adopted regimes which reveal the viability of our current model in the context of $f(R,T)$ modified gravity.

在这项研究中，我们的主要重点是研究大质量中子星的质量半径关系和几个重要性质，以了解目前此类致密天体的性质、行为和演化。此外，我们希望准确地理解核心核物质的状态方程及其稳定平衡构型。我们选择了一些巨大的双星脉冲星，并研究了它们的最大可达到质量和最小可能半径。我们将爱因斯坦-希尔伯特作用视为$F（右,\mathrm{时间}）=右+\alpha \mathrm{时间}$， 在哪里$右$是 Ricci 标量，$\mathrm{时间}$，能量动量张量的迹$\alpha$作为耦合参数，并使用修改后的 TOV 方程。球形中子星的内部时空与恒星表面的外部史瓦西线元相匹配。这$\mathrm{中号}$–$右$曲线可以预测最大可达到的质量约为$3。51{\mathrm{中号}}_{\odot }$尽可能最小的半径约为$10。5$km 为稳定平衡状态下的大质量致密恒星。我们已经通过加速时空获得了大质量中子星结构演化的清晰图像，并且可以对与之相关的几个量进行一些限制。从我们目前的调查中可以看出，所有派生的结果都与物理采用的制度相兼容，这揭示了我们当前模型在以下情况下的可行性：$F（右,\mathrm{时间}）$修正重力。