  While the presence of magnetic fields on low-mass stars is attributed to a
dynamo process essentially driven by convective motions, the existence of
magnetic fields on intermediate-mass stars has very likely other reasons.
Presuming that the fields we see are nearly constant in time, the paper focuses
on the generation of stable magnetic configurations at the early stages of
stellar evolution. The convective processing of an initial magnetic field
during the pre-main-sequence phase is studied in a very simple model star.
Azimuthal magnetic fields are found to be typical remnants in the upcoming
radiative envelope after the convection has receded.
