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 talk we present calculations of all four bulk viscosity coefficients assuming that they are "generated" by 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.

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