从重离子数据得到的软核物质状态方程及其对致密星的意义
Soft nuclear equation-of-state from heavy-ion data and implications for compact stars
摘要：
在亚阈能重离子碰撞中K介子产生的测量结果表明，当密度达到核物质饱和密度的2-3倍时，K介子的产生是一个软核物质状态方程。我们应用这些结果来研究紧凑型恒星性质的影响，特别是在最近测量的两个太阳质量脉冲星PSR J1614-2230的背景下。其意义有两个方面：首先，重离子的结果将核物质限制在与轻中子星相关的密度。因此，半径测量可以提供关于对称能的密度依赖性的信息，这是核物理中的一个关键量。其次，从重离子数据分析中得到的核子势信息可以与因果关系对核物质状态方程的限制相结合。由此我们可以推导出一个最大允许致密恒星质量的极限，即三个太阳质量。
英文摘要：
Measurements of kaon production at subthreshold energies in heavy-ion collisions point to a soft nuclear equation-of-state for densities up to 2-3 times nuclear matter saturation density. We apply these results to study the implications on compact star properties, especially in the context of the recent measurement of the two solar mass pulsar PSR J1614-2230. The implications are two-fold: Firstly, the heavy-ion results constrain nuclear matter at densities relevant to light neutron stars. Hence, a radius measurement could provide information about the density dependence of the symmetry energy which is a crucial quantity in nuclear physics. Secondly, the information on the nucleon potential obtained from the analysis of the heavy-ion data can be combined with restrictions from causality on the nuclear equation-of-state. From this we can derive a limit for the highest allowed compact star mass of three solar masses.
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