Equation of state and neutrino transfer in supernovae and neutron stars
Equation of state and neutrino transfer in supernovae and neutron stars
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DOI：
10.1140/epja/s10050-021-00644-z
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发表时间：
2021-12
期刊：
影响因子：
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通讯作者：
K. Sumiyoshi
中科院分区：
文献类型：
--
作者：
K. Sumiyoshi
本文综述了天体物理模拟用状态方程表和中微子输运数值计算方法的进展。炽热和致密的物质在核心坍缩的超新星和中子星中起着至关重要的作用。物态方程通过热力学量的行为来确定致密物体的结构和动力学。此外，中微子被困在超新星核心和中子星星合并中，并经常与物质相互作用，对决定爆炸机制和致密物体最终形式的动力学产生关键影响。因此，通过获得可靠的状态方程和反应速率数据集，在数值模拟中实现核和中微子物理的详细过程是至关重要的。我们展示了状态方程和中微子转移的发展的例子，并讨论了通过第一原理计算理解爆炸现象的研究方向。
We overview the progress of the tables of the equation of state for astrophysical simulations and the numerical methods of neutrino transfer. Hot and dense matter play essential roles in core-collapse supernovae and neutron stars. Equation of state determines the structure of compact objects and their dynamics through its behavior of thermodynamic quantities. In addition, neutrinos are trapped in supernova cores and neutron star mergers and frequently interact with matter to crucially affect dynamics in determining the explosion mechanism and the final form of compact objects. Therefore, it is essential to implement detailed processes of nuclear and neutrino physics in numerical simulations by having reliable data set of the equation of state and reaction rates. We show examples of developments of the equation of state and the neutrino transfer and discuss research directions toward understanding the explosive phenomena by the first principle calculation.