Convection in protoneutron stars and the structure of surface magnetic fields in pulsars

Details Convection in protoneutron stars and the structure of surface magnetic fields in pulsars Convection in protoneutron stars and the structure of surface magnetic fields in pulsars

2003-11-07

arxiv.org/abs/astro-ph/0311181v1

Astron.Astrophys. 415 (2004) 305-311

Astronomy and Astrophysics

Astrophysics

Scientific paper

10.1051/0004-6361:20034447

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 proto-neutron 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 about 10^{14} g/cm^{3} and then spreads to the surface. Because of high crustal conductivity, magnetic fields with the lengthscale about 1-3 km can survive in the crust as long as 10-100 Myr and form a sunspot-like structure at the surface of radiopulsars.

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