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arXiv 0704.1071astro-phnucl-th
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超流中子星的体粘滞系数

Bulk viscosity of superfluid neutron stars

M. E. Gusakov

备注：
11 pages, 1 figure, this version with some minor stylistic changes is published in Phys. Rev. D
发表信息：
Phys.Rev.D76:083001,2007
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摘要：

描述超流中子星动力学效应的流体力学与标准的单流体力学有本质的区别。特别是，我们在理论中有四个体积粘度系数，而不是一个。在本文中，我们计算这些系数，第一次，假设他们是由于非平衡β-过程（如修改或直接Urca过程）。我们的分析结果被用来估计超流中子星中声波的特征阻尼时间。它表明，所有四个体积粘性系数导致可比的声波耗散，并应考虑在同一个立足点。

英文摘要：

The hydrodynamics, describing dynamical effects in superfluid neutron stars, essentially differs from the standard one-fluid hydrodynamics. In particular, we have four bulk viscosity coefficients in the theory instead of one. In this paper we calculate these coefficients, for the first time, assuming they are due to non-equilibrium beta-processes (such as modified or direct Urca process). The results of our analysis are used to estimate characteristic damping times of sound waves in superfluid neutron stars. It is demonstrated that all four bulk viscosity coefficients lead to comparable dissipation of sound waves and should be considered on the same footing.

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