  Core collapse supernovae (SN) are the final stages of stellar evolution in
massive stars during which the central region collapses, forms a neutron star
(NS), and the outer layers are ejected. Recent explosion scenarios assumed that
the ejection is due to energy deposition by neutrinos into the envelope but
detailed models do not produce powerful explosions. There is mounting evidence
for an asphericity in the SN which is difficult to explain within this picture.
This evidence includes the observed high polarization, pulsar kicks, high
velocity iron-group and intermediate-mass elements material observed in
remnants, etc.
  The discovery of highly magnetars revived the idea that the basic mechanism
for the ejection of the envelope is related to a highly focused MHD-jet formed
at the NS. Our 3-D hydro simulations of the jet propagation through the star
confirmed that the mechanism can explain the asphericities.
  In this paper, detailed 3-D models for jet induced explosions of "classical"
core collapse supernovae are presented. We demonstrate the influence of the jet
properties and of the underlaying progenitor structure on the final density and
chemical structure. Finally, we discuss the observational consequences,
predictions and tests of this scenario.
