  In this paper we readdress the issue of the alignment of Classical T Tauri
stars with the magnetic field in the Taurus-Auriga molecular cloud. Previous
studies have claimed that the jet axis of active young stellar objects,
projected in the plane of the sky, is aligned preferentially along the
projected direction of the local magnetic field. We re-examine this issue in
view of the numerous high angular resolution images of circumstellar disks and
micro-jets now available. The images show that T Tauri stars as a group are
oriented randomly with respect to the local magnetic field, contrary to
previous claims. This indicates that the magnetic field may play a lesser role
in the final stages of collapse of an individual prestellar core than
previously envisioned. The current database also suggests that a subsample of
CTTS with resolved disks but without observations of bright and extended
outflows have a tendency to align perpendicularly to the magnetic field. We
discuss the possibility that this may trace a less favorable topology, e.g.,
quadrupolar, for the magnetic field in the inner disk, resulting in a weaker
collimated outflow.
