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Neutron star cooling with various superfluid and superconducting states

様々な超流動や超伝導状態を取り入れた場合の中性子星冷却

野田 常雄*; 橋本 正章*; 松尾 康秀*; 安武 伸俊*; 丸山 敏毅  ; 巽 敏隆*

Noda, Tsuneo*; Hashimoto, Masaaki*; Matsuo, Yasuhide*; Yasutake, Nobutoshi*; Maruyama, Toshiki; Tatsumi, Toshitaka*

A neutron star is a highly dense object which lasts after a supernova explosion. The density of a neutron star overcomes the nuclear density, and the temperature is high at the beginning of its history. An isolated neutron star does not have any heat sources, and it cools down emitting thermal energy by neutrinos. The neutrino emission process depends on the state of interior matter of the neutron star. To compare theoretical simulations and observations of neutron stars, it can constrain the nuclear theory of high density region. We create a model of neutron stars with colour superconducting quark matter and nucleon super fluidity / superconductivity, to satisfy recent observations, including two 2$$M$$$$_odot$$ neutron stars. We parameterize these super-states and demonstrate the cooling curves, which show heavy stars do not always cool faster than lighter stars.

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