  We present 3-d numerical magneto-hydrodynamic simulations of a buoyant,
twisted magnetic flux rope embedded in a stratified, solar-like model
convection zone. The flux rope is given an initial twist such that it neither
kinks nor fragments during its ascent. Moreover, its magnetic energy content
with respect to convection is chosen so that the flux rope retains its basic
geometry while being deflected from a purely vertical ascent by convective
flows. The simulations show that magnetic flux is advected away from the core
of the flux rope as it interacts with the convection. The results thus support
the idea that the amount of toroidal flux stored at or near the bottom of the
solar convection zone may currently be underestimated.
