  We present results of the first ever three-dimensional (3D)
magnetohydrodynamic (MHD) simulations of the accretion-ejection structure. We
investigate the 3D evolution of jets launched symmetrically from single stars
but also jets from warped disks in binary systems. We have applied various
model setups and tested them by simulating a stable and bipolar symmetric 3D
structure from a single star-disk-jet system. Our reference simulation
maintains a good axial symmetry and also a bipolar symmetry for more than 600
rotations of the inner disk confirming the quality of our model setup. We have
then implemented a 3D gravitational potential (Roche potential) due to a
companion star and run a variety of simulations with different binary
separations and mass ratios. These simulations show typical 3D deviations from
axial symmetry, such as jet inclination outside the Roche lobe or spiral arms
forming in the accretion disk. In order to find indication for precession
effects, we have also run an exemplary parameter setup, essentially governed by
a small binary separation of only $\simeq{200}$ inner disk radii. This
simulation shows strong indication that we observe the onset of a jet
precession caused by the wobbling of the jet launching disk. We estimate the
opening angle of the precession cone defined by the lateral motion of the the
jet axis of about 4 degree after about 5000 dynamical time steps.
