  We present full resolution (~0.2mas, ~0.1 A.U.) Very Long Baseline
Interferometry maps of the v=1, J=1-0 SiO masers in the Orion-KL nebula. The
morphology and turbulent nature of the maser emission argues against models in
which the masers form in an expanding and rotating protostellar disk. Rather,
we find that the symmetry evident in the SiO maser emission points towards its
genesis in a bipolar outflow. Water masers which also appear towards Orion-KL
are known to share the velocity profile and double peaked characteristics of
the SiO maser emission yet form much further away from the protostar. We link
the water masers to our present results by proposing that both species of maser
form around a flared molecular outflow of roughly constant velocity.
