Thermal Evolution of Neutron Stars and Hadronic Condensations

1. 介子凝聚和中子星的热演化：考虑到介子凝聚和核子超流动性导致的快速冷却，我们证明了观测的总体特征是可以解释的。我们还证明，轴子，如果真的存在的话，会产生特殊的T^4依赖于发射率，并在老中子星中与光子竞争。初生中子星的性质：我们首先构建了一个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（EOS）。基于这些结果，我们还给出了初始中子星半径和旋转速度的新约束条件。介子凝聚与中子星：我们在手性对称的基础上研究了介子凝聚相。随后，我们结合抑制高密度区域冷凝的相对论平均场理论，提出了一个最现实的状态方程。利用这个方程，我们讨论了中子星的体积性质和动力学过程；本文还讨论了伽玛暴和迷你黑洞情景的一些启示。k介子凝聚与中子星的热演化：我们已经证明直接的URCA过程在k介子凝聚阶段不一定是可能的，只在有限的密度区域起作用。我们还研究了核子在凝聚相中存在超流动性的可能性，发现这种可能性不大。此外，我们还指出并修正了前人关于介子凝聚体下中微子发射率的一个因子2的误差。

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.