The Vaidya and Tikekar (1982) ansatz has so far provided numerous stellar solutions which are useful for the description of compact stars like neutron stars and quark stars. We re-examine the impacts of the spacetime curvature parameter of the Vaidya–Tikekar ansatz on the physical properties of the relativistic anisotropic star. For a spherically symmetric, static and anisotropic stellar configuration, in the Vaidya–Tikekar background spacetime, we develop new exact solutions by assuming a polytropic type equation of state $p_r=k{\rho }^{1+\frac{1}{n}}-\beta$. Recent data from observed pulsars are taken as input parameters to validate the developed model. We examine the impact of the spheroidal curvature parameter of the VT spacetime on the stellar behaviour and mass–radius (M–R) relationship. It is observed that with the increase in the departure from spherical geometry, values of physical quantities, such as density and pressure, increase.

Vaidya 和 Tikekar (1982) ansatz 迄今为止提供了许多恒星解决方案，这些解决方案对于描述中子星和夸克星等致密恒星非常有用。我们重新研究 Vaidya-Tikekar ansatz 的时空曲率参数对相对论各向异性恒星物理性质的影响。对于球对称、静态和各向异性的恒星结构，在 Vaidya-Tikekar 背景时空中，我们通过假设多变型状态方程开发了新的精确解$p_r=k{\rho }^{1+\frac{1}{n}}-\beta$。来自观测到的脉冲星的最新数据被用作输入参数来验证所开发的模型。我们研究了 VT 时空的球体曲率参数对恒星行为和质量半径 (M-R) 关系的影响。据观察，随着偏离球面几何形状的增加，密度和压力等物理量的值增加。