论文标题
动荡的，固定的超丝体在中子星和脉冲星故障恢复中
Turbulent, pinned superfluids in neutron stars and pulsar glitch recoveries
论文作者
论文摘要
Pulsar的故障提供了对中子恒星高密度内部超级流体动力学的洞察力。但是，为了建模这些现象，需要了解通过固定晶格移动的湍流超流体涡流的动力学。在本文中，我们开发了一种理论方法来描述固定，湍流和旋转的超流体中涡流介导的相互摩擦。然后将我们的模型应用于Vela Pulsar和PSR J0537-6910中的毛刺后旋转进化的研究。我们表明，在这两种情况下，湍流模型都比层流相比拟合了自旋频率的演变。我们还预测，故障之后的频率的第二个导数应与以来以来的等待时间相关联，我们发现这与这些脉冲星的观察数据一致。本文的主要结论是，在这两个脉冲星的吉利克后旋转演化中，我们很可能观察到对恒星固定的湍流区域的响应（可能是地壳），而不是常规的直涡流阵列的层状响应。
Pulsar glitches offer an insight into the dynamics of superfluids in the high density interior of a neutron star. To model these phenomena, however, one needs to have an understanding of the dynamics of a turbulent array of superfluid vortices moving through a pinning lattice. In this paper we develop a theoretical approach to describe vortex mediated mutual friction in a pinned, turbulent and rotating superfluid. Our model is then applied to the study of the post glitch rotational evolution in the Vela pulsar and in PSR J0537-6910. We show that in both cases a turbulent model fits the evolution of the spin frequency derivative better than a laminar one. We also predict that the second derivative of the frequency after a glitch should be correlated with the waiting time since the previous glitch, which we find to be consistent with observational data for these pulsars. The main conclusion of this paper is that in the post-glitch rotational evolution of these two pulsars we are most likely observing the response to the glitch of a pinned turbulent region of the star (possibly the crust) and not the laminar response of a regular straight vortex array.
