Equation of State of Dense Supermova Matter and Newborm Hot Neutron Stays

本项目旨在获得致密超新星物质的热动力学量和物态方程的实际结果，并讨论新生热中子星的特征。此外，我们的目标是研究与超新星物质相关的富中子核物质的性质，以及不稳定核的基本物理学。(1)作为一种逼近有限温度核子物质的方法，我们提出了一种求解有限温度Hartree-Fock方程组的方法，并证明了该方法的有效性和可行性。特别是，“分离方法”，分离成一个现实的双核子部分和唯象部分V是非常有效的，看看结果是如何受到目前的理论不确定性。(2)本文列出了在较宽温度T、密度ρ和轻子分数y_l范围内的致密超新星物质的热力学量，并对组分布居常数、大质子分数Y_p和硬化状态方程等结果作了解释，指出Y_p可用公式Y_p=/Y_l+0.05表示，其精度在3%以内。(3)本文系统地研究了丰中子核物质的体质量和单粒子质量的ρ、T和α（不对称性）依赖性，讨论了核不可压缩性k的T和α依赖性。发现随着α的增大，液-气相变共存区变窄。(4)我们已经指出，新生中子星是“胖”的，因此自旋和结合能的释放预计在早期冷却阶段。结合SN 1987 A的中微子爆发讨论了中子星释放的能量，发现热中子星的诞生对通常冷中子星的最大质量和最大自转速率产生了新的约束.

In this project, we aimed to obtain realistic results of the thermo-dynamic quantities and the equation of state (EOS) for dense supernova matter and to discuss the characteristics of newborn hot neutron stars. Also, we aimed to investigate the properties of neutron-rich nuclear matter relevant to supernova matter, in connection with the underlying physics of unstable nuclei.(1) As a way to approach nucleon matter at finite temperature, we have proposed the method to solve a set of finite-temperature Hartree-Fock equations with the effective uncleon interaction V and shown the validity as well as the workability. In particular, the "separation method" to separate V into a realistic two-nucleon part and a phenomenological part is very effective to see how the results are affected by the present theoretical uncertainties.(2) We have tabulated the thermodynamic quantities of dense supernova matter for wide ranges of temperature T, denisty rho and lepton fraction y_l and given the explanations to the findings such as the constant population of the constituents, the large proton fraction Y_p and the stiffened EOS.It is remarked that Y_p is represented within 3% accuracy by the formula Y_p=/Y_l+0.05.(3) We have systematically investigated the rho-, T- and alpha (asymmetry)- dependences of the bulk and the single-particle quantities of neutron-rich nuclear matter and discussed the T- and the aipha- dependence of nuclear incompressibility k. It is found that the coexistent region for the Liquid-Gas phase transition becomes narrower as aipha increases.(4) We have ramarked that newborn neutron stars are "fat" and hence the spin-up and the release of binding energy are expected in the early cooling stage. The released energy is discussed in relation to the neutrino burst of SN1987A.It is found that hot neutron stars at birth bring about new constraints on the maximum mass and the maximum rotation rate of usual cold neutron stars.