具有相互摩擦的快速旋转超流中子星的流体动力学
Hydrodynamics of rapidly rotating superfluid neutron stars with mutual friction
摘要：
我们研究了超流中子星的时间演化，着重于振荡谱的性质、相互摩擦力对振荡的影响以及脉冲星毛刺的流体动力学自旋上升相。我们线性化的牛顿双流体模型的快速旋转的背景下的动力学方程。在轴对称平衡构型中，两个流体组分共转并且处于β平衡。我们使用分析状态方程生成分层和非分层恒星模型，这使我们能够研究系统的动力学自由度之间的耦合。通过线性化动力学方程的时间演化，我们确定了轴对称和非轴对称振荡模式的谱，考虑了引力位扰动的贡献，即不采用考林近似。我们研究了超流振荡的互摩擦阻尼，并考虑了互摩擦力的非耗散部分对模式频率的影响。我们还提供了Sidery，Passamonti和Andersson（2010）讨论的脉冲星毛刺的流体动力学模型的技术细节和相关测试。特别是，我们描述了用于生成模拟预毛刺状态的初始数据的方法，并推导出用于提取引力波信号的方程。
英文摘要：
We study time evolutions of superfluid neutron stars, focussing on the nature of the oscillation spectrum, the effect of mutual friction force on the oscillations and the hydrodynamical spin-up phase of pulsar glitches. We linearise the dynamical equations of a Newtonian two-fluid model for rapidly rotating backgrounds. In the axisymmetric equilibrium configurations, the two fluid components corotate and are in beta-equilibrium. We use analytical equations of state that generate stratified and non-stratified stellar models, which enable us to study the coupling between the dynamical degrees of freedom of the system. By means of time evolutions of the linearised dynamical equations, we determine the spectrum of axisymmetric and non-axisymmetric oscillation modes, accounting for the contribution of the gravitational potential perturbations, i.e. without adopting the Cowling approximation. We study the mutual friction damping of the superfluid oscillations and consider the effects of the non-dissipative part of the mutual friction force on the mode frequencies. We also provide technical details and relevant tests for the hydrodynamical model of pulsar glitches discussed by Sidery, Passamonti and Andersson (2010). In particular, we describe the method used to generate the initial data that mimic the pre-glitch state, and derive the equations that are used to extract the gravitational-wave signal.
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