  I propose a mechanism for axisymmetrical mass loss on the asymptotic giant
branch, that may account for the axially symmetric structure of elliptical
planetary nebulae. The proposed model operates for slowly rotating AGB stars,
having angular velocities of 0.0001 the Keplerian velocity. Such angular
velocities could be gained from a planet companion of mass 0.1M(Jupiter), or
even from single stars which are fast rotators on the main sequence. The model
assumes that dynamo magnetic activity results in the formation of cool spots,
above which dust forms much easily. The enhanced magnetic activity toward the
equator results in a higher dust formation rate there, and hence higher mass
loss rate. As the star ascends the AGB, both the mass loss rate and magnetic
activity increase rapidly, and hence the mass loss becomes more asymmetrical,
with higher mass loss rate closer to the equatorial plane.
