Symmetry coefficients and incompressibility of clusterized supernova matter

Clusterized nuclear matter in the (proto-)neutron star crust and the symmetry energy

Though generally agreed that the symmetry energy plays a dramatic role in determining the structure of neutron stars and the evolution of core-collapsing supernovae, little is known in what concerns its value away from normal nuclear matter density and, even more important, the correct definition of this quantity in the case of unhomogeneous matter. Indeed, nuclear matter traditionally addressed by mean-field models is uniform while clusters are known to exist in the dilute baryonic matter which constitutes the main component of compact objects outer shells. In the present work we investigate …

致密星中的团簇形成：相对论模型与Skyrme模型

Cluster formation in compact stars: relativistic versus Skyrme models

我们提出了各种性质的核和致密星物质，比较预测从两种唯象的方法：相对论模型（包括常数和密度依赖耦合）和非相对论Skyrme型相互作用。我们主要集中在液-气不稳定性，发生在欠饱和密度，导致分解的均匀物质成一个集群相。这种研究与中子星壳（零温度）和超新星动力学（有限温度）的描述有关。

基于核子相对论密度泛函的中子星物质广义描述

Generalised description of Neutron Star matter with nucleonic Relativistic Density Functional

本文基于相对论密度泛函提出核物质元建模方法，构建统一状态方程集合，并结合贝叶斯框架与天体物理观测约束中子星性质，重点揭示了同位旋矢量不可压缩性对高密度物质组成的影响。

Warm dense matter and cooling of supernovae remnants

We study the thermal effects on the nuclear matter (NM) properties such as binding energy, incompressibility, free symmetry energy and its coefficients using NL3, G3 and IU-FSU parameter sets of relativistic mean-field models. These models being consistent with the properties of cold NM, have also been used to study the effect of temperature by incorporating the Fermi function. The critical temperature for the liquid-gas phase transition in the symmetric NM is found to be 14.60, 15.37 and 14.50 MeV for NL3, G3 and IU-FSU parameter sets respectively, which is in excellent agreement with previou…

Thermal effects in hot and dilute homogeneous asymmetric nuclear matter

We present a comprehensive analysis of hot and dilute isospin-asymmetric nuclear matter employing the temperature-dependent effective-relativistic mean-field theory (E-RMF). The E-RMF is applied to study the effect of $δ$ and $ω-ρ$ meson cross-coupling on the thermal properties of asymmetric nuclear matter using two recently developed IOPB-I and G3 parameter sets. These sets are known to reproduce the nuclear matter properties in agreement with various experimental and observational constraints. We consider the nuclear matter to be homogeneous and study the equation of state (EoS) for densitie…

使用有限力程简单有效相互作用的热中子星物质状态方程

Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction

本文利用有限力程简单有效相互作用研究了热中子星物质在无中微子等温与有中微子俘获等熵条件下的状态方程，验证了抛物线近似的准确性，并分析了等熵线对斜率参数L的强依赖性及其对原中子星早期演化的影响。