Abstract
S22 is a peculiar supergiant in the Large Magellanic Cloud whose optical spectrum is characterized by numerous emission lines including Fell and [Fell] (Muratorio 1978). A detailed study performed by Friedjung and Muratorio (1980) led to two main conclusions: (a) A wind with a velocity of 70 km s-1 and a mass loss rate between 4x10-6 and 5x10-5 Mʘ yr-1 is suggested by the examination of the Balmer line P Cygni profiles, (b) The Fell and [Fell] emission lines come from a different region which is optically very thick in the permitted lines. Emission line curve-of-growth methods indicated that the region of line formation has a surface area perpendicular to the line of sight equal to that of a disk perpendicular to this direction with a radius between 3x1013 and 3x1014cm.
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