We study a model of the neutron star in \(\kappa \)-deformed space-time in the presence of the cosmological constant (\(\Lambda \)). The Einstein tensor and the energy-momentum tensor are generalized to \(\kappa \)-deformed space-time and we construct the field equations with the cosmological constant. Considering the interior of the star to be a perfect fluid as in the commutative case, we find the Tolman–Oppenheimer–Volkoff equations with the inclusion of the cosmological constant in \(\kappa \)-deformed space-time. The behavior of the maximum allowed mass of the star and its radius are studied with the variation in the cosmological constant as well as the deformation parameter. We see that the non-commutativity enhances the mass of the star and its maximum mass increases with a decrease in the cosmological constant. The maximum mass varies from 3.44 to \(3.68\,\text {M}_{\odot }\) as \(\Lambda \) varies from \(10^{-10}\) to \(10^{-15}\,\text {m}^{-2}\). We also obtain the compactness factor and surface redshift of the star. We observe that the compactness of the star increases as the cosmological constant decreases, whereas the surface redshift of the star decreases with a decrease in the cosmological constant. The compactness factor and surface redshift corresponding to the maximum mass of the neutron star remains almost constant as \(\Lambda \) decreases.

我们研究了存在宇宙常数 ( \(\Lambda \) ) 的\(\kappa \)变形时空中的中子星模型。将爱因斯坦张量和能量动量张量推广到kappa变形时空，并用宇宙学常数构造场方程。考虑到恒星内部在交换情况下是完美流体，我们找到了托尔曼-奥本海默-沃尔科夫方程，其中包含\(\kappa \)变形时空中的宇宙学常数。研究了恒星最大允许质量及其半径随宇宙学常数和形变参数变化的变化。我们看到，非交换性增强了恒星的质量，并且其最大质量随着宇宙常数的减小而增加。最大质量从 3.44 变化到\(3.68\,\text {M}_{\odot }\)，因为\(\Lambda \)从\(10^{-10}\)变化到\(10^{- 15}\,\文本{m}^{-2}\) .我们还获得了恒星的致密因子和表面红移。我们观察到，恒星的致密性随着宇宙学常数的减小而增加，而恒星的表面红移随着宇宙学常数的减小而减小。随着\(\Lambda \)减小，中子星最大质量对应的致密因子和表面红移几乎保持不变。