论文标题
原始中微子中微子 - 核子相互作用，原始中微子恒星的进化
Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions
论文作者
论文摘要
我们对带有球形对称性的新数值代码和使用准静态近似的新数值代码进行了原始中子星的开尔文 - 霍尔莫茨冷却阶段的模拟。我们首次使用全套带电的中微子核子反应，包括中子衰减和修饰的URCA过程，以及能量依赖性的数值表示，以包含具有随机相近似的核相关性。此外，在混合长度理论中考虑了对流动作。随着我们的计算中微子核子反应速率的假设，我们表明，对中微子驱动的风的冷却时间尺度，中微子信号和组成的主要影响来自包括对流运动。与平均场方法相比，随机相近似中核相关性的计算具有相对较小的影响。
We perform simulations of the Kelvin-Helmholtz cooling phase of proto-neutron stars with a new numerical code in spherical symmetry and using the quasi-static approximation. We use for the first time the full set of charged-current neutrino-nucleon reactions, including neutron decay and modified Urca processes, together with the energy-dependent numerical representation for the inclusion of nuclear correlations with random-phase approximation. Moreover, convective motions are taken into account within the mixing-length theory. As we vary the assumptions for computing neutrino-nucleon reaction rates, we show that the dominant effect on the cooling timescale, neutrino signal and composition of the neutrino-driven wind comes from the inclusion of convective motion. Computation of nuclear correlations within the random phase approximation, as compared to mean field approach, has a relatively small impact.
