Analysis of interplanetary magnetic field (IMF) data from the outer solar system has shown that the azimuthal component of the IMF falls off more rapidly with radius between 1 and 10 AU than as r-1, where an r-1 dependence is predicted in classical theory. This result is consistent with meridional flow transporting magnetic flux away from the heliographic equator. An identical effect has been predicted to result from the force due to the meridional gradient of the azimuthal component of the IMF. Here, the data are evaluated in the context of the theory and it is shown that the observed flux deficits generally agree with predictions by the MHD model. Furthermore, the MHD interaction is an attractive candidate for explaining the flux redistribution because it is conceptually simple and represents a direct body force on the plasma that does not depend on internal plasma processes. Important ingredients in the theory include the strength of the IMF, the magnitude of the solar wind flow speed, and possible meridional gradients in the flow speed, temperature, density, and radial field strength.