SUPERFLUID HYDRODYNAMICS IN ROTATING NEUTRON-STARS .1. NONDISSIPATIVE EQUATIONS

Newtonian hydrodynamic equations are developed 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. They also include the effects of rotation and forces due to the elastic properties of the neutron and proton vortices. The set of equations is closed by constructing a model of the total energy density and using it to express the dependent variables in terms of the independent variables. The low-frequency-long-wavelength limit of the equations is determined. The results will be applicable to studies of the large-scale oscillations of rotating and magnetized neutron stars.