We present a modeling of the thermal evolution of the neutron stars, incorporating an effect of neutron and proton pairing. The considered equation of state with induced surface tension (IST) reproduces properties of normal nuclear matter, fulfills the proton flow constraint, provides a high‐quality description of particle yields created in heavy‐ion collisions, and is equally compatible with the constraints from astrophysical observations and the GW170817 event. The model features strong direct Urca processes for the stars above 1.91 M_⊙. Our results show a very good agreement with the available cooling data, including observational data of the compact object in the center of the Cassiopeia A (Cas A), even without introducing nuclear pairing. The rapid cooling rate of the Cas A can be also reproduced by a 1.66 M_⊙ star with an atmosphere of light elements, high‐mass 1.955 − 1.96 M_⊙ stars with paired and unpaired matter, as well as by a 1.91 M_⊙ star with inclusion of neutron and proton pairings in the singlet channel.

中文翻译：

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用引起的表面张力在状态方程中描述中子星的热演化

我们提出了中子星热演化的模型，并结合了中子和质子配对的影响。考虑的具有诱导表面张力的状态方程（IST）再现了正常核物质的特性，满足了质子流约束，提供了重离子碰撞中产生的粒子产量的高质量描述，并且与天体物理学的约束同样兼容观测和GW170817事件。该模型功能强的直接Urca流程，天上的星星1.91 中号_⊙。我们的结果表明，即使不引入核对，现有的冷却数据也非常吻合，包括在仙后座A（Cas A）中心的紧凑物体的观测数据。在CAS A的快速冷却速率可通过也再现1.66 中号_⊙星与光元件，高质量的气氛1.96 - 1.955 中号_⊙恒星成对和不成问题，以及由1.91 中号_⊙与星在单线态通道中包括中子和质子对。