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Rapid postglitch spin-up of the superfluid core in pulsars
Alpar, M. A.; Langer, S. A.; Sauls, J. A.
AA(Columbia University, New York, NY; Illinois, University, Urbana, IL), AB(Princeton University, Princeton, NJ), AC(Princeton University, Princeton, NJ)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 15, 1984, p. 533-541. (ApJ Homepage)
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NASA/STI Keywords:
Magnetohydrodynamics, Neutron Stars, Pulsars, Stellar Cores, Stellar Rotation, Superfluidity, Drag, Electron Scattering, Stellar Magnetic Fields
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Vortex lines in the superfluid cores of neutron stars carry flux due to the induced proton charge current which results from the Fermi liquid interaction between neutrons and protons. As a consequence the scattering of charges off these magnetic vortex lines equilibrates the core superfluid to the plasma and the crust on time scales of order 1 second after a glitch. Thus, the core superfluid cannot be responsible for the observe time scales of the Vela and Crab pulsars. This result supports the theory of Alpar et al., in which both the glitch and the slow postglitch relaxation are determined by the interaction of vortices with nuclei in the crust.

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