标题： 具有三体力的微观核状态方程与中子星结构 显示英文标题

标题： Microscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure

摘要： 我们使用一种微观的不对称核物质状态方程（EOS）来计算非旋转中子星（NS）的静态性质。 该EOS是在Brueckner-Bethe-Goldstone多体理论框架下计算得到的。 为了重现核物质正确的饱和点，我们引入了三体力。 得到了一个微观且表现良好的EOS。 我们获得了一个最大质量构型，其质量为$M_{max} = 1.8 M_\odot$，半径为$R = 9.7$千米，中心密度为$n_c = 1.34~fm^{-3}$。 我们发现质子分数超过直接Urca过程起始的临界值$x^{Urca}$，在密度$n \geq 0.45~fm^{-3}$时。 因此，在我们的模型中，质量高于$M^{Urca} = 0.96 M_\odot$的中子星可以根据其中子超流性是否发生而经历非常快速的冷却。 与其他微观EOS模型进行了比较，并且也为这些模型计算了中子星结构。 显示英文摘要

摘要： We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter. The EOS is computed in the framework of the Brueckner--Bethe--Goldstone many--body theory. We introduce three-body forces in order to reproduce the correct saturation point of nuclear matter. A microscopic well behaved EOS is derived. We obtain a maximum mass configuration with $M_{max} = 1.8 M_\odot$, a radius $R = 9.7$ km and a central density $n_c = 1.34~fm^{-3}$. We find the proton fraction exceeds the critical value $x^{Urca}$, for the onset of direct Urca processes, at densities $n \geq 0.45~fm^{-3}$. Therefore, in our model, NS's with masses above $M^{Urca} = 0.96 M_\odot$ can undergo very rapid cooling depending on whether or not nucleon superfluidity in the interior of the NS takes place. A comparison with other microscopic models for the EOS is done, and neutron star structure is calculated for these models too.