论文标题
用于数值模拟的密集和热物质中中微子核子的相互作用改善
Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations
论文作者
论文摘要
中微子在紧凑型明星天体物理学中起着重要的作用：中微子加热是核心崩溃超新星中的主要成分之一，中微子的相互作用确定了二进制中子恒星合并中物质的组成，并且对重型元素核合成型和中子型核对体和中子的影响有很大的影响，除了中微子型核对体和中子恒星的状态外，中微子的相互作用是由中性型核能和中子恒星造成的。在过去的几十年中，许多作品都表明，在密集的物质中，培养基效应会大大改变中微子 - 物理的相互作用率，而许多天体物理模拟使用的分析近似通常远非再现更完整的计算。在这项工作中，我们提出了一个方案，该方案允许将带电的电流相互作用的提高速率纳入模拟中，并显示了核心折叠超新星的一些结果，其中在早期弹药后阶段的低能中微子中微子中中微子的中性中微子的位置存在明显的差异。
Neutrinos play an important role in compact star astrophysics: neutrino-heating is one of the main ingredients in core-collapse supernovae, neutrino-matter interactions determine the composition of matter in binary neutron star mergers and have among others a strong impact on conditions for heavy element nucleosynthesis and neutron star cooling is dominated by neutrino emission except for very old stars. Many works in the last decades have shown that in dense matter medium effects considerably change the neutrino-matter interaction rates, whereas many astrophysical simulations use analytic approximations which are often far from reproducing more complete calculations. In this work we present a scheme which allows to incorporate improved rates, for charged current interactions, into simulations and show as an example some results for core-collapse supernovae, where a noticeable difference is found in the location of the neutrinospheres of the low-energy neutrinos in the early post-bounce phase.
