核塌缩超新星的状态方程效应
Equation of state effects in core-collapse supernovae
摘要：
我们研究了核物质状态方程的不同性质对坍缩超新星的影响，重点研究了原中子星收缩及其对激波演化的影响。为此，我们引入了一系列的状态方程，改变核子的有效质量，不可压缩性，对称能，和核饱和点。这使我们能够指出从Lattimer和Swesty到Shen等人的状态方程（模拟中最常用的两个状态方程）改变这些属性的不同效果。特别是，我们跟踪收缩行为的有效质量，这决定了热核子状态方程的贡献。较大的有效质量导致较低的压力在核密度和较低的热指数。这导致了原中子星更快的收缩，从而导致更高的中微子能量，这有助于冲击波演化为更快的爆炸。
英文摘要：
We investigate the impact of different properties of the nuclear equation of state in core-collapse supernovae, with a focus on the proto-neutron-star contraction and its impact on the shock evolution. To this end, we introduce a range of equations of state that vary the nucleon effective mass, incompressibility, symmetry energy, and nuclear saturation point. This allows us to point to the different effects in changing these properties from the Lattimer and Swesty to the Shen et al. equations of state, the two most commonly used equations of state in simulations. In particular, we trace the contraction behavior to the effective mass, which determines the thermal nucleonic contributions to the equation of state. Larger effective masses lead to lower pressures at nuclear densities and a lower thermal index. This results in a more rapid contraction of the proto-neutron star and consequently higher neutrino energies, which aids the shock evolution to a faster explosion.
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