Resumen
The aim of our research will be to address why millisecond pulsars have relatively weak surface magnetic fields, of about 10^8, with a narrow spread. We propose that the accretion of plasma from the companion star fully screens the original neutron star field, but the accretion disk carries additional magnetic flux from the companion star, or itself can generate field by means of dynamo processes. This might lead to an asymptotic magnetic field of 10^8, as inferred from observations. When we are around a strongly magnetized star, the field prevents the disk from approaching the star. The accretion is along the field lines and deposits the matter on the polar cap of the star. Then, the accreted plasma flows, dragging with itself the magnetic field lines, from the pole to the equator. On the other hand, when the star becomes non magnetic, because the field has been buried, the disk is close to the star's surface and the transport is from the equator to the pole. We are interested in describing both processes and the final stationary state.
