超流退耦引起的年轻双星的转动演化
Rotational evolution of young pulsars due to superfluid decoupling
摘要：
脉冲星是旋转的中子星，被认为是慢下来的，自旋下降率被认为是由于磁偶极辐射。这导致对制动指数n的预测，其是旋转周期及其一阶和二阶时间导数的组合。然而，所有观察到的n值均低于预测值3。在这里，我们提供了一个简单的模型，可以解释的旋转演化的年轻的脉冲星，包括n=2.51的958岁的脉冲星在蟹状星云。该模型是基于有效的转动惯量的减少，由于在恒星的核心，成为超流体的恒星冷却通过中微子排放的比例增加。这些结果表明，未来对中子星的大型无线电监测活动将产生对中子星质量、核物质状态方程和超流体性质的测量。
英文摘要：
Pulsars are rotating neutron stars that are seen to slow down, and the spin-down rate is thought to be due to magnetic dipole radiation. This leads to a prediction for the braking index n, which is a combination of spin period and its first and second time derivatives. However, all observed values of n are below the predicted value of 3. Here we provide a simple model that can explain the rotational evolution of young pulsars, including the n=2.51 of the 958-year-old pulsar in the Crab nebula. The model is based on a decrease in effective moment of inertia due to an increase in the fraction of the stellar core that becomes superfluid as the star cools via neutrino emission. The results suggest that future large radio monitoring campaigns of pulsars will yield measurements of the neutron star mass, nuclear equation of state, and superfluid properties.
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