超流超子体粘滞系数与旋转中子星的r模不稳定性
Superfluid hyperon bulk viscosity and the r-mode instability of rotating neutron stars
摘要：
为了确定旋转中子星中不稳定的r模是否提供了一个可探测的引力波源，我们需要了解许多倾向于抵消不稳定性的耗散过程的细节。已经确定的是，由于外来粒子，如超子的体积粘度，在这方面可能是特别重要的。然而，超子超流性的影响至今还没有被完全解释。虽然相关的抑制的反应速率，引起的体积粘度已被估计，超流体方面的流体动力学没有被考虑。在本文中，我们确定的r-模式不稳定窗口的中子星与$Σ^{-}$超子核心，使用适当的多流体形式主义，包括，第一次，“超流体”的整体粘度系数的影响。我们证明，即使额外的条款可能会增加体积粘度阻尼有点，他们的存在并不影响的r-模式不稳定窗口的定性特征。
英文摘要：
In order to establish whether the unstable r-modes in a rotating neutron star provide a detectable source of gravitational waves, we need to understand the details of the many dissipative processes that tend to counteract the instability. It has been established that the bulk viscosity due to exotic particles, like hyperons, may be particularly important in this respect. However, the effects of hyperon superfluidity have so far not been fully accounted for. While the associated suppression of the reaction rates that give rise to the bulk viscosity has been estimated, superfluid aspects of the fluid dynamics have not been considered. In this paper we determine the r-mode instability window for a neutron star with a $Σ^{-}$ hyperon core, using the appropriate multifluid formalism including, for the first time, the effect of the "superfluid" bulk viscosity coefficients. We demonstrate that, even though the extra terms may increase the bulk viscosity damping somewhat, their presence does not affect the qualitative features of the r-mode instability window.
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