Statistics – Computation
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..261u&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 2, May 15, 1992, p. 261-268.
Statistics
Computation
53
Neutron Stars, Ohmic Dissipation, Stellar Evolution, Stellar Magnetic Fields, Stellar Temperature, Computational Astrophysics, Cooling, Electric Current, Surface Layers
Scientific paper
The hypothesis that the neutron star magnetic field is initially confined to the near-surface layers of the crust is examined. It is shown that the neutron star cooling can effectively increase the conductivity, sigma, and the characteristic ohmic decay time, tau(B). At the initial stage the field decays comparatively rapidly: it can decrease by a factor of 10-100 during the first 10 exp 6 - 10 exp 7 yr depending on initial field location. At this stage the conductivity is determined by electron-phonon scattering. After about 10 exp 6 - 10 exp 7 yr, sigma in the crust begins to be determined by the scattering on impurities and may be sufficiently high in pure crystals. At late stages tau(B) is largely due to the higher conductivity, and it can increase during the evolution because of magnetic field diffusion into the deep layers of the crust. It is shown that the crustal field decays rather slowly even in the case when the field is initially confined to the outer regions of the crust.
Muslimov Alex G.
Urpin Vadim A.
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