耗散旋转超流中子星中的波动和不稳定性
Waves and instabilities in dissipative rotating superfluid neutron stars
摘要：
本文讨论了旋转超流中子星核中的波的传播，并考虑了涡旋介导的相互摩擦力。对于两种流体在未扰动状态下共同旋转的模型，我们的分析澄清了化学耦合和夹带声波和惯性波的作用。我们还研究了相互摩擦阻尼，提供的结果表明，众所周知的事实，即声波沿涡流阵列传播是无阻尼的。我们表明，这是不正确的惯性波，这是阻尼的相互摩擦，无论传播方向。然后，我们包括涡张力，这是由于局部涡曲率。专注于纯粹的横向惯性波，我们推导出小的修正，张力诱导波的频率。最后，我们允许背景中的相对线性流动（沿着旋转轴）。在这种情况下，我们展示了如何相互摩擦耦合可能会引起惯性波的动力学不稳定性。我们讨论了临界流所需的不稳定性，它的物理解释和可能的相关性，它可能有中子星物理。
英文摘要：
We discuss wave propagation in rotating superfluid neutron star cores, taking into account the vortex mediated mutual friction force. For models where the two fluids co-rotate in the unperturbed state, our analysis clarifies the role of chemical coupling and entrainment for sound and inertial waves. We also investigate the mutual friction damping, providing results that demonstrate the well-known fact that sound waves propagating along a vortex array are undamped. We show that the same is not true for inertial waves, which are damped by the mutual friction regardless of the propagation direction. We then include the vortex tension, which arises due to local vortex curvature. Focussing on purely transverse inertial waves, we derive the small correction that the tension induces in the wave frequency. Finally, we allow for a relative linear flow in the background (along the rotation axis). In this case we show how the mutual friction coupling may induce a dynamical instability in the inertial waves. We discuss the critical flow required for the instability to be present, its physical interpretation and the possible relevance it may have for neutron star physics.
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