Yasin H, Schäfer S, Arcones A, Schwenk A
Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany.
ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany.
Phys Rev Lett. 2020 Mar 6;124(9):092701. doi: 10.1103/PhysRevLett.124.092701.
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.
我们研究了核状态方程的不同性质在核心坍缩超新星中的影响，重点关注原中子星的收缩及其对激波演化的影响。为此，我们引入了一系列状态方程，这些方程在核子有效质量、不可压缩性、对称能和核饱和点方面有所不同。这使我们能够指出从拉蒂默和斯韦斯蒂状态方程到沈等人的状态方程（模拟中最常用的两种状态方程）改变这些性质时的不同效果。特别是，我们将收缩行为追溯到有效质量，有效质量决定了对状态方程的热核子贡献。更大的有效质量导致在核密度下压力更低且热指数更低。这导致原中子星收缩更快，从而中微子能量更高，这有助于激波演化为更快的爆炸。
