  We investigate the generation of intrinsically asymmetric or {\it one-sided}
outflows or jets from disk accretion onto rotating stars with complex magnetic
fields using axisymmetric (2.5D) magnetohydrodynamic simulations.
  The intrinsic magnetic field of the star is assumed to consist of a
superposition of an aligned dipole and an aligned quadrupole in different
proportions. The star is assumed to be rapidly rotating in the sense that the
star's magnetosphere is in the propeller regime where strong outflows occur.
Our simulations show that for conditions where there is a significant
quadrupole component in addition to the dipole component, then a dominantly
{\it one-sided} conical wind tends to form on the side of the equatorial plane
with the larger value of the intrinsic axial magnetic field at a given
distance. For cases where the quadrupole component is absent or very small, we
find that dominantly one-sided outflows also form, but the direction of the
flow "flip-flops" between upward and downward on a time-scale of $\sim 30$ days
for a protostar. The average outflow will thus be symmetrical. In the case of a
pure quadrupole field we find symmetric outflows in the upward and downward
directions.
