论文标题
具有超新星中微子的中微子的质量和半径的新方法
A New Approach to Mass and Radius of Neutron Stars with Supernova Neutrinos
论文作者
论文摘要
中子恒星在核心溢出的超新星爆炸中形成，其中发射了大量中微子。在本文中，计算了触发恒星的冷却阶段的超新星中微子光曲线，该恒星持续了几分钟。在数值模拟中，采用了90个具有不同不压缩性，对称能量和核子有效质量的状态现象学方程模型进行全面研究。发现对于具有较大的中子星质量和较小的中子星半径的模型，冷却时间尺度的时间更长。此外，冷却时间尺度的理论表达是作为质量和半径的函数提出的，并且发现它忠实地描述了数值结果。这些发现表明，可以使用中微子信号诊断新形成的中子星的质量和半径。
Neutron stars are formed in core-collapse supernova explosions, where a large number of neutrinos are emitted. In this paper, supernova neutrino light curves are computed for the cooling phase of protoneutron stars, which lasts a few minutes. In the numerical simulations, 90 models of the phenomenological equation of state with different incompressibilities, symmetry energies, and nucleon effective masses are employed for a comprehensive study. It is found that the cooling timescale is longer for a model with a larger neutron star mass and a smaller neutron star radius. Furthermore, a theoretical expression of the cooling timescale is presented as a function of the mass and radius and it is found to describe the numerical results faithfully. These findings suggest that diagnosing the mass and radius of a newly formed neutron star using its neutrino signal is possible.
