Neutron star magnetic field decay - Hall drift and Ohmic diffusion

Details Neutron star magnetic field decay - Hall drift and Ohmic diffusion Neutron star magnetic field decay - Hall drift and Ohmic diffusion

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.233..875j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 233, Aug. 15, 1988, p. 875-885.

Astronomy and Astrophysics

Astronomy

43

Drift Rate, Hall Effect, Magnetic Diffusion, Magnetic Flux, Neutron Stars, Stellar Magnetic Fields, Binary Stars, Cool Stars, Electrical Resistivity

Scientific paper

The paper reconsiders two problems relevant to the transport of magnetic flux in the solid crust. First, it is shown that below the neutron-drip threshold density, there is little diffusion of the Boltzmann gas of neutrons at temperatures less than about 10 to the 10th K. Nuclear abundances form under the equilibrium constraint that the mean baryon number per nucleus is independent of temperature. The equilibrium nuclear species have two different atomic numbers. The two-component plasma formed remains miscible as the star cools. The electrical conductivity, below the lattice Debye temperature, is much smaller than previously assumed, producing rapid Ohmic diffusion of magnetic flux at densities below the neutron-drip threshold. Secondly, it is proposed that the magnetic buoyancy force in the neutron-drip solid produces Hall drift of the magnetic flux analogous to the motion of vortices in the interior proton superconductor (Jones, 1975). The 5 Myr time constant observed in field decay is determined principally by the radial Hall drift velocity. With decreasing magnetic flux density, Hall drift becomes negligible and Ohmic diffusion in the neutron-drip solid is the cause of field changes at 10 greater than about 1000 Myr.

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