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Nuclear theory for neutron stars and supernovae

中子星和超新星的核理论

基本信息

批准号：
3303-2011
负责人：
Pearson, JohnMichael
金额：
$ 1.09万
依托单位：
Université de Montréal
依托单位国家：
加拿大
项目类别：
Subatomic Physics Envelope - Individual
财政年份：
2014
资助国家：
加拿大
起止时间：
2014-01-01 至 2015-12-31
项目状态：
已结题

来源：
https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=544094
关键词：
Nuclear theory neutron stars supernovae

项目摘要

The project described here is concerned with providing a unified treatment of the nuclear physics of supernovae, neutron stars and the r-process of nucleosynthesis. Neutron stars are formed in the aftermath of a supernova explosion, and the r-process may take place either simultaneously with the birth of the neutron star, or much later as our neutron star encounters some other compact star. The r-rocess is responsible for the synthesis of about a half of all nuclei in the universe heavier than iron, and all those heavier than bismuth (including notably uranium). The synthesis by this process even of stable nuclei 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, especially the mass, essential for a full understanding of the r-process. Our approach to this problem is to calculate nuclear masses from effective nuclear forces, i.e., forces with free parameters that have been adjusted to reproduce the masses of known nuclei. At the same time, these effective forces can be used to calculate the properties of the nuclear matter of which neutron stars and supernova cores consist. We are thus opening the way to a much more unified treatment of a vast range of nuclear-astrophysical phenomena than has been possible in the past.

这里描述的项目是关于提供一个统一的处理超新星，中子星和核合成的r-过程的核物理。中子星是在超新星爆炸后形成的，r-过程可能与中子星星的诞生同时发生，也可能在我们的中子星星遇到其他致密的星星时发生。宇宙中大约一半比铁重的原子核和所有比铋重的原子核（尤其是铀）都是由r过程合成的。即使是稳定核的合成过程也要经过中间阶段，中间阶段涉及的核非常不稳定，在实验室中无法观察到，因此只有通过理论才能对这些核的性质形成任何概念，特别是质量，这对于充分理解r-过程至关重要。我们解决这个问题的方法是从有效核力计算核质量，即，具有自由参数的力，这些力已被调整以再现已知原子核的质量。同时，这些有效力可以用来计算中子星和超新星核心组成的核物质的性质。因此，我们正在开辟一条道路，以一种比过去可能的更统一的方式来处理广泛的核天体物理现象。