Abstract
ABSTRACT The phenomenon of high-velocity molecular gas in regions of star formation is now known to be rather common. More than 60 cases have been reported in the literature. About one-half of the observed outflows exhibit a bipolar morphology, that is, the blueshifted and redshifted emitting zones appear located symmetrically with respect to the central source of excitation. The author reviews the following proposed collimating mechanisms: (1) The exciting star has a wind that is collimated from the stellar surface. (2) The isotropic wind of the exciting star is collimated by a circumstellar structure. (3) The isotropic wind of the exciting star is collimated by an interstellar structure. (4) The outflows are produced by a bipolar hydromagnetic wind.
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