Bulk viscosity of superfluid neutron stars

Abstract

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.

11 pages, 1 figure, this version with some minor stylistic changes is published in Phys. Rev. D

References in corpus (4)

• The entrainment matrix of a superfluid neutron-proton mixture at a finite temperature
• Temperature-dependent pulsations of superfluid neutron stars
• Constraining a possible time-variation of the gravitational constant through "gravitochemical heating" of neutron stars
• Rotochemical Heating of Neutron Stars: Rigorous Formalism with Electrostatic Potential Perturbations

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• The relativistic entrainment matrix of a superfluid nucleon-hyperon mixture at zero temperature
• Bulk viscosity in kaon-condensed color-flavor locked quark matter
• Bulk viscosity of superfluid hyperon stars
• Damping of sound waves in superfluid nucleon-hyperon matter of neutron stars
• Transport theory for cold relativistic superfluids from an analogue model of gravity
• Temperature effects in pulsating superfluid neutron stars
• Leptonic contribution to the bulk viscosity of nuclear matter
• Bulk viscosity coefficients due to phonons and kaons in superfluid color-flavor locked quark matter
• Hydrodynamic fluctuations in relativistic superfluids
• Classical and relativistic dynamics of supersolids: variational principle