Superfluid hydrodynamics in rotating neutron stars. I - Nondissipative equations. II - Dissipative effects

This paper presents Newtonian hydrodynamic equations which describe the outer-core regions of neutron stars composed of superfluid neutrons, superconducting protons, and degenerate electrons and muons. The equations include couplings to the gravitational and electromagnetic fields and also the effects of rotation and forces due to the elastic properties of the neutron and proton vortices. The LF-long-wavelength limit of the equations is determined. The equations are also generalized to include dissipation. The effects of viscosity, thermal conductivity, and mutual friction are included. The LF-long-wavelength limit is taken to obtain a set of equations suitable for studies of p-modes in rapidly rotating neutron stars. An energy functional is constructed which determines the damping times due to the various forms of dissipation.