Formation of color superconducting quark matter in supernovae and protoneutron stars

超新星和原中子星中彩色超导夸克物质的形成

• 批准号: 147172132
• 负责人: Dr. Giuseppe Pagliara
• 金额: --
• 依托单位: Institut für Theoretische Physik
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2009
• 资助国家: 德国
• 起止时间: 2008-12-31 至 2010-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/147172132?language=en
• 关键词: Formation; color; superconducting; quark; matter

The study of the properties of strongly interacting matter at finite density is the main subject of this project. In the last years a huge effort has been done to predict the structure of the QCD phase diagram at large densities with the result that different color superconducting phases can take place depending on the temperature and the baryonic chemical potential. If a color superconducting phase is really realised in Nature the only place in which it can be formed is the core of neutron stars where densities of order of ten times the nuclear matter saturation density are reached. The formation process of the color superconducting matter should occur during the collapse of the core of massive stars triggered by the increase of the central density of the star or during the cooling, by neutrino emission, of the newly born neutron stars. The dynamics of the collapse and the diffusion process and luminosity of neutrinos could be strongly influenced if color superconducting phases are formed during the early stages of the life of a compact star. The goal of this project is to provide possible signatures of the formation of quark phases in protoneutron stars which could be tested by the present neutrino detectors in the next core collapse supernova events in our galaxy (or in the local group of galaxies with the new generation of neutrino detectors planned).

研究有限密度下强相互作用物质的性质是本课题的主要课题。在过去的几年里，人们做了大量的工作来预测大密度下QCD相图的结构，结果是不同颜色的超导相可以根据温度和重子化学势而发生。如果在自然界中真的实现了彩色超导相，那么它唯一可以形成的地方就是中子星的核心，在那里密度达到核物质饱和密度的十倍。彩色超导物质的形成过程应该发生在由恒星中心密度增加引起的大质量恒星核心坍缩或新生中子星因中微子发射而冷却的过程中。如果在致密恒星生命的早期阶段形成彩色超导相，则会强烈影响中微子的坍缩动力学和扩散过程以及光度。该项目的目标是提供质子中子星中夸克相形成的可能特征，这些特征可以在我们银河系的下一个核心坍缩超新星事件中（或在计划中的新一代中微子探测器的局部星系群中）由现有的中微子探测器进行测试。