标题： 近期由短程关联范德瓦尔斯型模型重现的天体物理观测？ 显示英文标题

标题： Recent astrophysical observations reproduced by a short-range correlated van der Waals-type model?

摘要： 我们在一个范德瓦尔斯型模型中进行了改进，包括短程关联（SRC）效应。 假定核子间相互作用的吸引力和排斥力为密度相关的函数，更具体地说，我们采用Carnahan-Starling（CS）方法来描述后者，并为前者选择适当的表达式以再现Clausius（C）真实气体模型的结构。 结果显示，由此得到的模型（命名为CCS-SRC模型）的参数化能够重现对称核物质高密区压缩模量值在$K_0=(240\pm 20)$MeV范围内的流约束。 在星体物质的背景下，我们的研究指出CCS-SRC模型与最近的天体物理观测数据有很好的一致性，即来自GW170817和GW190425事件的引力波数据以及NASA的Neutron星内部组成探测器（NICER）任务提供的质量-半径轮廓、无量纲潮汐变形区域和数值。 此外，该模型对对称能斜率（$L_0$）的估值与最近发现的这个量的范围一致，据称该范围与更新后的铅半径实验（PREX-2）合作组报告的结果一致。 在这种情况下，更高的$L_0$值是优选的，而相反的情况则不允许模型与天体物理数据同时兼容。 显示英文摘要

摘要： We perform an improvement in a van der Waals-type model by including it effects of short-range correlations (SRC). Attractive and repulsive parts of the nucleon-nucleon interaction are assumed to be density-dependent functions, more specifically, we adopt the Carnahan-Starling (CS) method for the latter, and a suitable expression for the former in order to reproduce the structure of the Clausius (C) real gas model. The parametrizations of the resulting model, named as CCS-SRC model, are shown to be capable of reproducing the flow constraint at the high-density regime of symmetric nuclear matter for incompressibility values inside the range of $K_0=(240\pm 20)$ MeV. In the context of stellar matter, our findings point out a good agreement of the CCS-SRC model with recent astrophysical observational data, namely, mass-radius contours and dimensionless tidal deformability regions and values, coming from gravitational waves data related to the GW170817 and GW190425 events, and from the NASA's Neutron star Interior Composition Explorer (NICER) mission. Furthermore, the values for the symmetry energy slope of the model ($L_0$) are in agreement with a recent range found for this quantity, claimed to be consistent with results reported by the updated lead radius experiment (PREX-2) collaboration. In this case, higher values of $L_0$ are favored, while the opposite scenario does not allow simultaneous compatibility between the model and the astrophysical data.