  A radiation-driven disk wind model is proposed that offers great promise of
explaining the extreme mass loss signatures of massive young stellar objects
(the BN-type objects and more luminous Herbig Be stars). It is argued that the
dense low-velocity winds associated with young late-O/early-B stars would be
the consequence of continuing optically-thick accretion onto them. The launch
of outflow from a Keplerian disk allows wind speeds of about 200 km/s that are
substantially less than the escape speed from the stellar surface. The star
itself is not required to be a rapid rotator. Disk irradiation is taken into
account in the hydrodynamical calculation presented, and identified as an
important issue both observationally and from the dynamical point of view.
