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引起的快速冷却，我们证明了观测的总体特征是可以解释的。我们还表明，如果真的存在轴子，它会带来发射率的特殊T^4依赖关系，并与旧中子星中的光子轴子竞争。刚刚诞生的原中子星的性质：我们首先建立了一个处理超新星物质的理论框架，然后给出了它的化学成分和状态方程。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。Kaon凝聚和中子星：我们在手征对称性的基础上研究了Kaon凝聚相。随后，我们结合了抑制高密度区凝聚的相对论平均场理论，给出了一个最符合实际的状态方程。利用这个状态方程，我们讨论了中子星的整体性质和动力学过程，并讨论了对伽马射线爆发和小黑洞情况的一些启示。Kaon凝聚和中子星的热演化：我们已经证明，直接的Urca过程在Kaon凝聚相不一定是可能的，只在有限密度区起作用。我们还研究了凝聚态中核子超流的可能性，发现它是不可能的。此外，我们还通过前人关于介子凝聚态下中微子发射率的研究，指出并纠正了因子2的错误。

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.