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We use the magnetic butterfly diagram to determine the speed of the magneticflux transport on the solar surface towards the poles. The manifestation of theflux transport is clearly visible as elongated structures extended from thesunspot belt to the polar regions. The slopes of these structures are measuredand interpreted as meridional magnetic flux transport speed. Comparison withthe time-distance helioseismology measurements of the mean speed of themeridional flows at the depth of 3.5--12 Mm shows a generally good agreement,but the speeds of the flux transport and the meridional flow are significantlydifferent in areas occupied by the magnetic field. The local circulation flowsaround active regions, especially the strong equatorward flows on theequatorial side of active regions affect the mean velocity profile derived byhelioseismology, but do not influence the magnetic flux transport. The resultsshow that the mean longitudinally averaged meridional flow measurements byhelioseismology may not be used directly in solar dynamo models for describingthe magnetic flux transport, and that it is necessary to take into account thelongitudinal structure of these flows.

Speed of Meridional Flows and Magnetic Flux Transport on the Sun