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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：
2011
资助国家：
加拿大
起止时间：
2011-01-01 至 2012-12-31
项目状态：
已结题

来源：
https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=473685
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.

这里描述的项目涉及提供超新星、中子星的核物理和核合成的r过程的统一处理。中子星是在超新星爆炸后形成的，r过程可能与中子星的诞生同时发生，也可能在我们的中子星与其他致密恒星相遇时发生。宇宙中约有一半的原子核比铁重，所有比铋重的原子核(尤其是铀)都是由r-rocess合成的。通过这个过程合成稳定的核也要经过中间阶段，这些核是如此不稳定，以至于在实验室里无法观察到，所以只有通过理论，人们才能对这些核的性质，特别是质量，形成对充分理解r过程至关重要的任何概念。我们解决这个问题的方法是根据有效核力计算核质量，即具有自由参数的力，这些力已经被调整以重现已知原子核的质量。同时，这些有效力可以用来计算由中子星和超新星核组成的核物质的性质。因此，我们正在开辟一条比过去更统一地处理广泛的核-天体物理现象的道路。