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We present the first 3D MHD study in spherical geometry of the non-lineardynamical evolution of magnetic flux tubes in a turbulent rotating convectionzone. We study numerically the rise of magnetic toroidal flux ropes from thebase of a modelled convection zone up to the top of our computational domainwhere bipolar patches are formed. We compare the dynamical behaviour of fluxtubes in a fully convective shell possessing self-consistently generated meanflows such as meridional circulation and differential rotation, with referencecalculations done in a quiet isentropic zone. We find that two parametersinfluence the tubes during their rise through the convection zone: the initialfield strength and amount of twist, thus confirming previous findings inCartesian geometry. Further, when the tube is sufficiently strong with respectto the equipartition field, it rises almost radially independently of theinitial latitude (either low or high). By contrast, weaker field cases indicatethat downflows and upflows control the rising velocity of particular regions ofthe rope and could in principle favour the emergence of flux through Omega-loopstructures. For these latter cases, we focus on the orientation of bipolarpatches and find that sufficiently arched structures are able to create bipolarregions with a predominantly East-West orientation. Meridional flow seems todetermine the trajectory of the magnetic rope when the field strength has beensignificantly reduced near the top of the domain. Finally differential rotationmakes it more difficult for tubes introduced at low latitudes to reach the topof the domain.

Three dimensional non-linear evolution of a magnetic flux tube in a spherical shell: Influence of turbulent convection and associated mean flows