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 5x1 0-5M⊙ 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 3x1013and 3x1014cm.
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References
Bath, G.T., Pringle, J.E., Whelan, A.J. 1980, Mon. Not. R.A.S. 190, 185
Friedjung, M., Muratorio, G. 1980, Astron. Astrophys. 85, 233
Muratorio, G. 1978, Astron. Astrophys. Suppl. Ser. 33, 125
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© 1981 D. Reidel Publishing Company
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Muratorio, G., Bensammar, S., Cassatella, A., Friedjung, M., Viotti, R. (1981). The Ultraviolet to Infrared Spectrum of the Large Mass Loss LMC Supergiant S22 = HD 34664+. In: Chiosi, C., Stalio, R. (eds) Effects of Mass Loss on Stellar Evolution. Astrophysics and Space Science Library, vol 89. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8500-1_37
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DOI: https://doi.org/10.1007/978-94-009-8500-1_37
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