Crustal magnetic field evolution and neutron star cooling

Details Crustal magnetic field evolution and neutron star cooling Crustal magnetic field evolution and neutron star cooling

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992azh....69.1028u&link_type=abstract

Astronomicheskij Zhurnal (ISSN 0004-6299), vol. 69, no. 5, p. 1028-1040.

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Neutron Stars, Stellar Envelopes, Stellar Evolution, Stellar Magnetic Fields, Boundary Value Problems, Computational Astrophysics, Stellar Temperature

Scientific paper

Consideration is given to the magnetic field decay of neutron stars concentrated initially in relatively shallow layers of the crust with densities of 4 x 10 exp 11 g/cu cm. It is shown that neutron star cooling can effectively increase the conductivity of the crust and the ohmic decay time scale. A scenario of crustal field evolution is described. If the electric currents were initially concentrated within layers with a density of about (2-4) x 10 exp 11 g/cu cm, then the surface field decays by a factor of 100 to 1000 after about 10 exp 10 yr.

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