标题： r模与快速旋转超流中子星中的相互摩擦 显示英文标题

标题： r-modes and mutual friction in rapidly rotating superfluid neutron stars

摘要： 我们开发了一种新的微扰框架来研究旋转超流中子星的r模。我们的分析考虑了恒星的离心变形，并在扰动速度的一阶中考虑了两流体动力学。我们的主要重点是一种简单的模型系统，在该系统中总密度分布是一个$n=1$多态。我们推导出了经典r模超流体类比的部分解析解。此解用于分析涡旋介导的相互摩擦阻尼的相关性，确认这种耗散机制不太可能抑制快速旋转超流体中子星的引力波驱动不稳定性。我们的超流体r模计算比以前的方法简单得多，因为它从系统的其他惯性模式中解耦了r模。这使得结果更加清晰，但也意味着我们无法评论对于特定参数值可能发生（以及相关的“共振”）的潜在避免交叉的相关性。我们的相互摩擦阻尼分析与以前的研究有两个重要的不同之处。首先，我们采用了现实的配对间隙，这意味着恒星核心中的超流体区域随温度变化。其次，我们允许相互摩擦参数取所有允许的值，而不是专注于某一特定机制。因此，我们不仅考虑弱拖曳区域，还考虑强拖曳区域，其中流体力学显著不同。 显示英文摘要

摘要： We develop a new perturbative framework for studying the r-modes of rotating superfluid neutron stars. Our analysis accounts for the centrifugal deformation of the star, and considers the two-fluid dynamics at linear order in the perturbed velocities. Our main focus is on a simple model system where the total density profile is that of an $n=1$ polytrope. We derive a partially analytic solution for the superfluid analogue of the classical r-mode. This solution is used to analyse the relevance of the vortex mediated mutual friction damping, confirming that this dissipation mechanism is unlikely to suppress the gravitational-wave driven instability in rapidly spinning superfluid neutron stars. Our calculation of the superfluid r-modes is significantly simpler than previous approaches, because it decouples the r-mode from all other inertial modes of the system. This leads to the results being clearer, but it also means that we cannot comment on the relevance of potential avoided crossings (and associated "resonances") that may occur for particular parameter values. Our analysis of the mutual friction damping differs from previous studies in two important ways. Firstly, we incorporate realistic pairing gaps which means that the regions of superfluidity in the star's core vary with temperature. Secondly, we allow the mutual friction parameters to take the whole range of permissible values rather than focussing on a particular mechanism. Thus, we consider not only the weak drag regime, but also the strong drag regime where the fluid dynamics is significantly different.