Fermion zero-mode influence on neutron-star magnetic field evolution
Corresponding Author
P. B. Jones
Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH
E-mail: [email protected]Search for more papers by this authorCorresponding Author
P. B. Jones
Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH
E-mail: [email protected]Search for more papers by this authorABSTRACT
The quantum phenomenon of spectral flow which has been observed in laboratory superfluids, such as 3He-B, controls the drift velocity of proton type II superconductor vortices in the liquid core of a neutron star and so determines the rate at which magnetic flux can be expelled from the core to the crust. In the earliest and most active phases of the anomalous X-ray pulsars and soft-gamma repeaters, the rates are low and consistent with a large fraction of the active crustal flux not linking the core. If normal neutrons are present in an appreciable core matter-density interval, the spectral flow force limits flux expulsion in cases of rapid spin-down, such as in the Crab pulsar or in the propeller phase of binary systems.
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