  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.
