Nuclear theory for collapsed stars and r-process nucleosynthesis

这里描述的项目是关于提供r过程的核物理的统一理论解释。这是一个发生在剧烈的恒星事件中的过程，如引力坍缩超新星或中子星合并，并且负责宇宙中一半的原子核的核合成，这些原子核属于比铁更重的元素，以及所有比铋更重的元素（特别是铀）。即使是稳定的核，r过程的合成也要经过中间阶段，这些中间阶段涉及的核是如此不稳定，以至于在实验室中无法观察到，因此只有通过理论，人们才能对这些核的性质形成任何概念，这对于充分理解这个过程是必不可少的。我们特别关心的核性质是结合能和裂变。在通过中子-星星合并合成r过程核的情况下，中子星星壳的状态方程的知识是必不可少的，并且我们已经能够将我们已经发展的核结合能理论推广到这个问题。

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.