In order to solve the Tolman-Oppenheimer-Volkoff equations for neutron stars, one routinely uses the equations of state which are computed in the Minkowski spacetime. Using a first-principle approach, it is shown that the equations of state which are computed within the curved spacetime of the neutron stars include the effect of gravitational time dilation. It arises due to the radially varying interior metric over the length scale of the star and consequently it leads to a much higher mass limit. As an example, for a given set of parameters in a $\sigma -\omega$ model of nuclear matter, the maximum mass limit is shown to increase from $1.61M_{\odot }$ to $2.24M_{\odot }$ due to the inclusion of gravitational time dilation.

中文翻译：

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弯曲时空状态方程中中子星的更高质量极限

为了求解中子星的 Tolman-Oppenheimer-Volkoff 方程，人们通常使用在 Minkowski 时空计算的状态方程。使用第一性原理方法，表明在中子星弯曲时空内计算的状态方程包括引力时间膨胀的影响。它是由于恒星长度尺度上径向变化的内部度量而产生的，因此它导致了更高的质量限制。例如，对于给定的一组参数$\sigma -\omega$ 核物质模型，最大质量限制显示从 $1.61{米}_{\odot }$ 到 $2.24{米}_{\odot }$ 由于包含了引力时间膨胀。