Volume 415, Number 1, February III 2004
|Page(s)||305 - 311|
|Section||Stellar structure and evolution|
|Published online||03 February 2004|
Convection in protoneutron stars and the structure of surface magnetic fields in pulsars
A.F. Ioffe Institute of Physics and Technology and Isaak Newton Institute of Chili, Branch in St. Petersburg, 194021 St. Petersburg, Russia
2 Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain
3 Institute of Astronomy, University of Zielona Gora, Lubuska 2, 65-265 Zielona Gora, Poland
Corresponding author: V. Urpin, firstname.lastname@example.org
Accepted: 3 November 2003
We consider generation and evolution of small-scale magnetic fields in neutron stars. These fields can be generated by small-scale turbulent dynamo action soon after the collapse when the protoneutron star is subject to convective and neutron finger instabilities. After instabilities stop, small-scale fields should be frozen into the crust that forms initially at high density ~ 1014 g/cm3 and then spreads to the surface. Because of high crustal conductivity, magnetic fields with the lengthscale ~ km can survive in the crust as long as 10–100 Myr and form a sunspot-like structure at the surface of radiopulsars.
Key words: stars: pulsars: general / stars: neutron / magnetic fields
© ESO, 2004
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