  The periodic precession (162--day) and nodding (6.3--day) motions of the jets
in SS433 are driven in the outer regions of the disc, whereas the jets
themselves, being relativistic, are launched near the black hole at the disc
centre. Given that the nutation period is comparable to the dynamical timescale
in the outer regions of the disc, it seems unlikely that these periods can be
communicated efficiently to the disc centre. Here we propose that the massive
outflow observed in SS433 is launched at large radii in the disc, about 1/10 of
the outer disc edge, and that it is this outflow which responds to the
oscillations of the outer disc and determines the direction of the jets. The
massive outflow is launched at large radius because the mass transfer rate is
hyper-Eddington. This implies not only that the total luminosity of SS433
exceeds $\le$ by a considerable factor, but also that the radiative output is
collimated along the outflow. We thus suggest that SS433 is an ultraluminous
X-ray source (ULX) viewed `from the side'. We also suggest that the obscured
{\it INTEGRAL} sources may be SS433--like objects, but with slightly lower mass
transfer rates.
