  We compute successfully the launching of two magnetic winds from two
circumbinary disks formed after a common envelope event. The launching is
produced by the increase of magnetic pressure due to the collapse of the disks.
The collapse is due to internal torques produced by a weak poloidal magnetic
field. The first wind can be described as a wide jet, with an average mass-loss
rate of $\sim 1.3 \times 10^{-7}$ \Moy\ and a maximum radial velocity of $\sim
230$ \kms. The outflow has a half-opening angle of $\sim 20^{\circ}$. Narrow
jets are also formed intermittently with velocities up to 3,000 \kms, with
mass-loss rates of $\sim 6 \times 10^{-12} $ \Moy\ during short periods of
time. The second wind can be described as a wide X-wind, with an average
mass-loss rate of $\sim 1.68 \times 10^{-7}$ \Moy\ and a velocity of $\sim 30$
\kms. A narrow jet is also formed with a velocity of 250 \kms, and a mass-loss
rates of $\sim 10^{-12} $ \Moy.
  The computed jets are used to provide inflow boundary conditions for
simulations of proto-planetary nebulae. The wide jet evolves into a molecular
collimated outflow within a few astronomical units, producing proto-planetary
nebulae with bipolar, elongated shapes, whose kinetic energies reach $\sim 4
\times 10^{45}$ erg at 1,000 years. Similarities with observed features in
W43A, OH231.8+4.2, and Hen 3-1475 are discussed.
  The computed wide X-wind produces proto-planetary nebulae with slower
expansion velocities, with bipolar and elliptical shapes, and possible starfish
type and quadrupolar morphology.
