Nuclear theory for collapsed stars and r-process nucleosynthesis

这里描述的项目是关于为r过程的核物理学提供一个统一的理论处理。这是一个发生在剧烈恒星事件中的过程，比如超新星的引力坍缩或中子星合并，它负责宇宙中一半的原子核的核合成，这些原子核属于比铁重的元素，以及所有比铋重的元素（尤其是铀）。即使是稳定的原子核，r过程合成也要经过中间阶段，其中包括一些不稳定的原子核，它们无法在实验室中观察到，所以只有通过理论，人们才能形成对这些原子核性质的任何概念，这对充分理解这个过程至关重要。我们特别关心的核性质是结合能和裂变。在通过中子星合并合成r过程核的情况下，中子星地壳状态方程的知识是必不可少的，并且我们已经能够将我们发展的核结合能理论扩展到这个问题。

The project described here is concerned with providing a unified theoretical treatement  of the nuclear physics of the r-process. This is a process occurring in violent stellar events such as gravitational-collapse supernovas or neutron-star mergers, and is responsible for the nucleosynthesis of half of all the nuclei in the universe belonging to elements heavier than iron, and all those heavier than bismuth (including notably uranium). The r-process synthesis even of nuclei that are stable passes through intermediate stages involving nuclei that are so unstable that they cannot be observed in the laboratory, so that it is only through theory that one can form any idea of the properties of these nuclei, essential for a full understanding of the process. The nuclear properties with which we are notably concerned are binding energy and fission. In the case of the synthesis of r-process nuclei through neutron-star mergers a knowledge of the equation of state of the neutron star's crust is essential, and we have been able to extend to this problem the theory that we have developed for nuclear binding energies.