In the present work, we investigate the bulk properties of nuclear matter and neutron stars with the newly proposed relativistic parametrizations HPUA, HPUB and HPUC which provides an opportunity to readjust the coupling parameters keeping in view the properties of finite nuclei, nuclear matter and astrophysical constraints. The HPUA, HPUB and HPUC are proposed by fitting both PREX-II + CREX results simultaneously, PREX-II and CREX results for neutron skin thickness of ²⁰⁸Pb and ⁴⁸Ca respectively to assess their implications. The relativistic parameterizations have been generated by including non linear self-interactions of σ and ω- mesons and mixed interactions of ω, and ρ-meson up to the quartic order. The new equations of state (EoSs) composed of nucleons and leptons in β - equilibrium are constructed with the newly proposed parameter sets. The maximum mass of the neutron star by employing the EoSs computed with the HPU's parameter sets lies in the range $2.02\pm 0.03$ M⊙ - $2.04\pm 0.03$ M⊙ and the radius of canonical neutron star ($R_{1.4}$) comes out to be equal to $12.89\pm 0.08$ Km - $13.27\pm 0.30$ Km (including BPS crust). The value of dimensionless tidal deformability, for canonical mass, is $590.83\pm 22.58$ - $631.52\pm 78.13$ which satisfies the constraints of waveform models analysis of GW170817. A covariance analysis is also performed to calculate the statistical uncertainties in the model parameters and nuclear matter observables along with their correlations.

在目前的工作中，我们利用新提出的相对论参数化 HPUA、HPUB 和 HPUC 研究核物质和中子星的整体特性，这提供了重新调整耦合参数的机会，同时考虑到有限核、核物质和天体物理约束的特性。HPUA、HPUB 和 HPUC 是通过同时拟合 PREX-II + CREX 结果而提出的，PREX-II 和 CREX 结果分别针对²⁰⁸ Pb 和⁴⁸ Ca 的中子皮厚度来评估其影响。相对论参数化是通过包含σ和ω - 介子的非线性自相互作用以及ω和ρ的混合相互作用而生成的-介子达到四次阶。用新提出的参数集构建了处于β平衡的核子和轻子组成的新状态方程 (EoS) 。通过使用 HPU 参数集计算出的 EoS，中子星的最大质量位于以下范围内$2.02\pm 0.03$M⊙ -$2.04\pm 0.03$M⊙ 和规范中子星的半径（${右}_{1.4}$) 结果等于$12.89\pm 0.08$公里-$13.27\pm 0.30$公里（包括 BPS 地壳）。对于规范质量，无量纲潮汐变形能力值为$590.83\pm 22.58$-$631.52\pm 78.13$满足GW170817波形模型分析的约束条件。还进行协方差分析来计算模型参数和核物质可观测值的统计不确定性及其相关性。