Crustal Entrainment and Pulsar Glitches
arXiv:1210.8177 · doi:10.1103/PhysRevLett.110.011101
Abstract
Large pulsar frequency glitches are generally interpreted as sudden transfers of angular momentum between the neutron superfluid permeating the inner crust and the rest of the star. Despite the absence of viscous drag, the neutron superfluid is strongly coupled to the crust due to non-dissipative entrainment effects. These effects are shown to severely limit the maximum amount of angular momentum that can possibly be transferred during glitches. In particular, it is found that the glitches observed in the Vela pulsar require an additional reservoir of angular momentum.
5 pages, 3 figures, revised version
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- Pulsar Glitches: The Crust may be Enough
- Pulsar spin-down: the glitch-dominated rotation of PSR J0537-6910
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- Magnetic Field Generation in Stars
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- Anti-glitches within the standard scenario of pulsar glitches
- Neutron Star Physics in the Square Kilometer Array Era : An Indian Perspective
- Constraints on neutron skin thickness in 208Pb and density-dependent symmetry energy
- Superfluid instability of r-modes in "differentially rotating" neutron stars
- Nuclear Energy Density Functionals: What do we really know?
- Slowly rotating superfluid neutron stars with isospin dependent entrainment in a two-fluid model
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