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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.利用真实核力研究超新星爆炸后刚诞生的热中子星的性质我们研究了热中子星的性质，计算了它们演化过程中的能量释放和自旋加速比。2.有限温度下的K介子凝聚和质子中子星我们根据手征对称性提出了一个在K介子凝聚相中引入量子涨落和热涨落的框架，并导出了状态方程。解TOV方程得到了质子中子星的平衡位形，从而讨论了延迟坍缩成黑洞的可能性。3.非平衡状态下K介子凝聚的出现和增长我们详细研究了化学非平衡状态下动力学相变的特征，指出热K介子的产生和湮灭反应速率在其它过程中占主导地位4. π凝聚、大质子混合和超子超流下的核子超流性及其对中子星冷却的影响将已有的理论推广到包含DELTA同量异位素自由度，我们发现DELTA使π ^0凝聚的临界温度和存在区域增大，而使π ^C凝聚的临界温度和存在区域减小。在大质子混合的情况下，质子对也会凝聚，净效应对中子星星冷却并不有效。5.对最近的Gamow-Teller共振和π介子凝聚实验的重新研究我们利用最近从巨Gamow-Teller共振得到的信息重新研究了π介子凝聚的可能性。因此，我们指出，它应该在中子星和重离子反应的背景下认真重新考虑。