  I reexamine recent observations of velocity profiles across jets blown by
young stellar objects, and argue that the observations do not support the
interpretation of jets rotating around their symmetry axes. Instead, I propose
that the interaction of the jets with a twisted-tilted (wrapped) accretion disk
can form the observed asymmetry in the jets' line of sight velocity profiles.
The proposed scenario is based on two plausible assumptions. (1) There is an
inclination between the jet and the outer parts of the disk; the jet is
perpendicular to the inner part of the disk; Namely, there is a twisted-tilted
(wrapped) disk. (2) The disk-jet interaction slows down the jet as the jet
entrains mass from the disk, with larger decelaration of jet segments closer to
the tilted disk. The proposed scenario can account for the basic properties of
the observed velocity profiles, while having the advantage that there is no
need to refer to any magnetic jet launching model, and there is no need to
invoke jet rotation with a huge amount of angular momentum.
