权益分类	功能权益	普通用户	{{item.name}}会员
{{category.name}}	{{benefitItem.name}}

Kaon condensation and Neutron stars

卡翁凝聚和中子星

基本信息

批准号：
08640369
负责人：
TATSUMI Toshitaka
金额：
$ 1.41万
依托单位：
KYOTO UNIVERSITY
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
1996
资助国家：
日本
起止时间：
1996 至 1998
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-08640369/
关键词：
Neutron stars Equation of state Protoneutron stars Phase transition Kaon condensation Pion condensation Hyperon superfluidity Delayed collapse カイラル対称性核子超流動超新星高エネルギー重イオン反応

项目摘要

1.Proper ties of hot neutron stars just born after supernova explosions by the use of a realistic nuclear forceWe studied the properties of hot neutron stars and calculated the energy release and spin-up ratio during their evolution.2.Kaon condensation at finite temperature and protoneutron starsWe proposed a framework to introduce quantum and thermal fluctuations in the kaon condensed phase on the basis of chiral symmetry, and derived the equation of state. Solving the TOV equation we obtained the equilibrium configuration of protoneutron stars and thereby discussed the possibility of the delayed collapse to black holes.3.Appearance and growth of kaon condensation under nonequilibriumWe studied in detail the characteristic features of the dynamic phase transition under chemical nonequilibrium and pointed out that the reaction rates for creation and annihilation of thermal kaons are dominant over those of other processes before and after phase transition.4.Nucleon superfluidity under pion condensation or large proton-mixing and hyperon superfluidity, and their implications on neutron-star coolingExtending the privious theory to include the DELTA isobar degrees of freedom, we found that the critical temperature and the existing region are increased due to DELTA for pi^0 condensation ; while those are reduced for pi^C condensation. In the case of large proton mixing, where proton pairs condense as well, the net effect is not efficient for neutron star cooling. A hyperon superfluidity is also studied.5.Recent experiment on Gamow-Teller resonance and pion condensation reexaminedWe reexamined the possibility of pion condensation by using the recent information from giant Gamow-Teller resonance. Consequently we remarked that it should be seriously re-considered in the context of neutron stars and heavy-ion reactions.

1.利用真实核力超新星爆炸后诞生的热中子星的性质我们研究了热中子星的性质，计算了其演化过程中的能量释放和自旋比。2.有限温度下的Kaon凝聚和原中子星我们提出了一个基于手性对称性的框架，在Kaon凝聚相中引入量子和热涨落，并推导出状态方程。求解TOV方程得到了原中子星的平衡构型，从而讨论了延迟塌缩成黑洞的可能性。3.非平衡下kaon凝聚的出现和生长详细研究了化学非平衡下动态相变的特征，指出热kaon产生和湮灭的反应速率优于化学非平衡前后的其他过程。 4.π介子凝聚或大质子混合和超子超流性下的核子超流性及其对中子星冷却的影响将先前的理论扩展到包括DELTA等压线自由度，我们发现由于DELTA，π^0凝聚的临界温度和现有区域有所增加；而这些则因π^C缩合而被还原。在大量质子混合的情况下，质子对也会凝聚，净效应对于中子星冷却来说并不有效。还研究了超子超流性。5.重新审视伽莫夫-泰勒共振和π介子凝聚的最新实验利用巨伽莫夫-泰勒共振的最新信息，重新审视了π介子凝聚的可能性。因此，我们认为应该在中子星和重离子反应的背景下认真重新考虑它。