Superfluid Core Rotation in Pulsars. I. Vortex Cluster Dynamics

Abstract

view Abstract Citations (88) References (57) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Superfluid Core Rotation in Pulsars. I. Vortex Cluster Dynamics Sedrakian, Armen D. ; Sedrakian, David M. Abstract Starting from conservation laws, a magnetohydrodynamic theory for rotating neutron-proton superfluid mixture in neutron star cores is formulated. The theory incorporates the effects of energy dissipation and mutual friction. In particular, the equations of motion of uncoupled neutron and proton vortices in the bulk and at the boundaries of the superfluid core are derived. As a result of the entrainment of superconducting proton currents by the superfluid neutron vortex circulation, rotation induced supercurrents and magnetic fields are generated in the neutron-proton superfluid mixture. The magnetic field enters the vicinity of each neutron vortex line by forming a triangular two- dimensional lattice (vortex cluster) confined around the neutron vortex line within a macroscopic length scale δn ∼ 10-5 cm. The net number of proton vortices bound in each vortex cluster is found to be <np> ∼ 1012-1013, producing a mean magnetic field induction of the cluster <Bc> 1014 G. The axisymmetric magnetic field induction averaged over the core of neutron star is of order <B> 1011-1012 G. This is a generated component of neutron star magnetic field, which in contrast to a possible fossil field of the star, is independent of its magnetic history prior to the nucleation of the superconducting phase and nucleation process as well. The arrangement of vortices in clusters imposes constraints on the equations of motion of uncoupled vortices. We determine the effective dynamical equations of motion of vortex clusters by establishing the form of effective Magnus and frictional forces. Vortex cluster friction is dominated by the scattering of relativistic electrons from magnetic field of proton vortices and leads to a strong coupling of the clusters to the normal electron liquid. The resulting dynamical coupling times are found to be from few days to 103 days for different density regions of the superfluid core. These timescales are compatible with the observed postjump relaxation times of pulsars. Publication: The Astrophysical Journal Pub Date: July 1995 DOI: 10.1086/175876 Bibcode: 1995ApJ...447..305S Keywords: DENSE MATTER; MAGNETOHYDRODYNAMICS: MHD; STARS: INTERIORS; STARS: NEUTRON; STARS: PULSARS: GENERAL full text sources ADS | Related Materials (1) Part 2: 1995ApJ...447..324S