Issue |
A&A
Volume 415, Number 1, February III 2004
|
|
---|---|---|
Page(s) | 305 - 311 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20034447 | |
Published online | 03 February 2004 |
Convection in protoneutron stars and the structure of surface magnetic fields in pulsars
1
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, vadim.urpin@uv.es
Received:
6
October
2003
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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