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Phase Transition of High Density Matter in the Universe

宇宙中高密度物质的相变

基本信息

批准号：
60302024
负责人：
SATO Katsuhiko
金额：
$ 3.39万
依托单位：
University of Tokyo
依托单位国家：
日本
项目类别：
Grant-in-Aid for Co-operative Research (A)
财政年份：
1985
资助国家：
日本
起止时间：
1985 至 1987
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-60302024/
关键词：
Cosmology Early Universe Supernova Neutron Star 相転移ニュートリノ Highlights of Astronomy

项目摘要

Results of the present research are summarized in the following three group. 1) Early Universe: A new method for quantum cosmology, in which the time is explicitly appeared and the probability is always positive definite, was formulated (Hosoya). Baryogenesis in the inflationary universe was investigated systematically. It was found that i) non thermal effects in the reheating stage play an important role, ii) in the chaotic inflationary scenario, baryon number domain structure might be formed (Sato). Evolution of density fluctuations which are formed by the phase transition in the early universe was investigated and the constraints on the model imposed from the homogeneity of 3k background radiation was made clear (Sasaki). Nucleosynthesis in the lepton-number asymmetric universe was investigated and it was found that more stringent constraints on the asymmetry is obtained.2) Supernova and Neutron Star: Theoretical analysis of neutrino burst from the Supernova 1987A was made and it was found that i) the burst is surprisingly consistent with theoretical prediction, ii) The mass of neutron star just born might be 1.2-1.6M, iii) The mass of electron type neutrinos mast be smaller than 26 eV (Sato). Monte Calro simulation of finite temperature quark gluon plasma was made and it was found that the transition is of first order (UKawa).3) High density plasma: Two phase separation (hydrogen and iron ions) in the center of the sun was investigated and it was found this separation does not occur (Ichimaru). Neutrino loss rate was calculated in detail on the basis of Weinberg-Salam theory (Itoh).

本研究的结果总结为以下三组。1)早期宇宙：提出了一种新的量子宇宙学方法(Hosoya)，在该方法中，时间显式出现，概率总是正定的。系统地研究了膨胀宇宙中的重子发生。结果表明：1)重加热阶段的非热效应起着重要作用；2)在混沌暴涨的情况下，可能会形成重子数域结构(Sato)。研究了早期宇宙相变形成的密度涨落的演化，明确了3k背景辐射的均匀性对模型的限制(Sasaki)。研究了轻子数不对称宇宙中的核合成，得到了对非对称性更严格的约束。2)超新星和中子星：对超新星1987A中微子爆发进行了理论分析，发现：1)中微子爆发与理论预测惊人地一致；2)刚刚诞生的中子星的质量可能是1.2-1.6米；3)电子型中微子的质量必须小于26 eV(Sato)。对有限温度夸克胶子等离子体进行了蒙特卡罗模拟，发现跃迁是一级的(Ukawa)。3)高密度等离子体：研究了太阳中心的两相分离(氢离子和铁离子)，发现这种分离没有发生(Ichiaru)。根据Weinberg-Salam理论(Itoh)详细计算了中微子损失率。