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Thermal Evolution of Neutron Stars and Hadronic Condensations

中子星和强子凝聚的热演化

基本信息

批准号：
06640388
负责人：
TATSUMI Toshitaka
金额：
$ 1.34万
依托单位：
KYOTO UNIVERSITY
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (C)
财政年份：
1994
资助国家：
日本
起止时间：
1994 至 1995
项目状态：
已结题

项目摘要

1. Pion condensation and thermal evolution of neutron stars : Taking into account the rapid cooling due to pion condensate and nucleon superfluidity, we have shown that gross feature of observation can be explained. We have also shown that axions, if really exist, bring about the peculiar T^4 dependense of the emissivity, and competes with the photon one in old neutron stars.2. Properties of proto-neutron stars just born : We have first constructed a theoretical framework to treat the supernova-matter, and then presented its chemical composition and equation of state (EOS). Based on these results, we have also given new constraints on the radius and rotational velocity of initial neutron stars.3. Kaon condensation and neutron stars : We have studied kaon condensed phase on the basis of chiral symmetry. Subsequently we have presented a most realistic equation of state, by incorporating the relativistic mean-field theory which supress the condensation at high-density region. Using this EOS we have discussed the bulk properties and dynamical processes of neutron stars ; some implications on the gamma-ray bursts and mini black-hole scenario are also discussed.4. Kaon condensation and the thermal evolution of neutron stars : We have shown that the direct URCA process is not necessarily possible in the kaon condensed phase and works only in the limited density region. We have also examined the possibility of nucleon superfluidity in the condensed phase, and found that it is unlikely.In addition we have pointed out and corrected an error of factor 2 through the previous studies about the neutrino emissivity under the meson condensates.

1.π介子凝聚和中子星的热演化：考虑到π介子凝聚和核子超流性引起的快速冷却，我们已经证明了观测的总体特征是可以解释的。我们还证明了轴子，如果真的存在的话，会导致发射率的特殊的T^4依赖性，并与老中子星中的光子发射率竞争。初生原中子星的性质：我们首先建立了处理超新星物质的理论框架，然后给出了它的化学组成和状态方程。基于这些结果，我们还对初始中子星的半径和自转速度给出了新的约束. K介子凝聚和中子星：我们在手征对称性的基础上研究了K介子凝聚相。随后，我们结合相对论平均场理论，提出了一个最符合实际的物态方程，它抑制了高密度区的凝聚。利用这个状态方程，我们讨论了中子星的体性质和动力学过程，并讨论了对伽玛射线暴和小黑洞的一些启示. K介子凝聚和中子星的热演化：我们已经表明，直接URCA过程不一定是可能的K介子凝聚相和工程只在有限的密度区域。我们还考察了凝聚相中核子超流性的可能性，发现它是不可能的，另外，我们还指出并纠正了前人关于介子凝聚下中微子发射率的研究中的一个2倍的错误。