快速旋转超流中子星中的r模和相互摩擦
r-modes and mutual friction in rapidly rotating superfluid neutron stars
摘要：
我们发展了一个新的微扰框架来研究旋转超流中子星的r模。我们的分析帐户的离心变形的恒星，并认为两个流体动力学在线性顺序的扰动速度。我们的主要重点是在一个简单的模型系统中的总密度分布是一个$n=1$ polytrope。我们推导出一个部分解析解的超流模拟的经典r-模式。这个解决方案是用来分析的涡旋介导的相互摩擦阻尼的相关性，确认这种耗散机制是不可能抑制的引力波驱动的不稳定性在快速旋转的超流中子星。我们的计算的超流体r-模式是显着简单比以前的方法，因为它从所有其他惯性模式的系统的r-模式。这使得结果更加清晰，但也意味着我们不能评论可能发生的特定参数值的潜在避免交叉（和相关的“共振”）的相关性。我们的相互摩擦阻尼的分析不同于以前的研究在两个重要的方面。首先，我们将现实的配对差距，这意味着该地区的超流性在恒星的核心随温度而变化。其次，我们允许相互摩擦参数采取整个范围的允许值，而不是集中在一个特定的机制。因此，我们不仅考虑了弱阻力区，而且考虑了流体动力学显著不同的强阻力区。
英文摘要：
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.
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