the peculiar bipolar H II region S106, which otherwise shows all the characteristics of a massive YSO (Drew et al. 1993), has radio emission elongated perpendicular to the outflow axis (Hoare et al. 1994; Hoare & Muxlow 1996; Hoare 2002). S140 IRS 1 also has such an equatorial wind of about 500 AU in size (Hoare & Muxlow 1996; Hoare 2002). Originally interpreted as a jet (Schwartz 1989; Tofani et al. 1995) it is clearly perpendicular to the large scale bipolar molecular outflow and to the monopolar IR reflection nebula at the base of the blueshifted outflow cavity revealed in speckle observations (Schertl et al. 2000; Alvarez et al. 2004). Proper motions confirm that this structure is not moving outwards as would be expected for a jet (Hoare 2002). Another possible example of an equatorial wind is in GL490 (Campbell et al. 1986), although the extension in the radio emission along the disc plane (Mundy & Adelman 1988) is somewhat noisy.

To drive such equatorial winds it has been proposed by Drew et al. (1998) that the radiation pressure due to central star and inner disc act on the ionized gas at the surface of the disc. The gas is 