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Dust Driven Winds in Late Supergiants

Published online by Cambridge University Press:  12 April 2016

Erwin Sedlmayr ,
Carsten Dominik  and
Hans-Peter Gail
Erwin Sedlmayr
Affiliation:
Institut für Astronomie und Astrophysik Technische Universität Berlin Hardenbergstraβe 36, D-1000 Berlin 12
Carsten Dominik
Affiliation:
Institut für Astronomie und Astrophysik Technische Universität Berlin Hardenbergstraβe 36, D-1000 Berlin 12
Hans-Peter Gail
Affiliation:
Institut für Theoretische Astrophysik Universität Heidelberg Im Neuenheimer Feld 561, 6900 Heidelberg 1

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The oool extended shells of giants and supergiants are well known to be places of copious dust formation as indicated by the occurrence of pronounced extinction, reddening, and polarization of the continuous star light and by the appearance of particular absorption features, both manifesting the interaction of photons with particles considerably larger than atoms or molecules.

The accepted explanation of these phenomena is the formation of circumstellar dust, i.e. small solid particles with a typical size of the order of 0.1 micron. However, the analysis of these effects yields only information on the interaction of photons with certain functional groups within the clusters - e.g. Si-O, C-H, C-C bending and Si-O, C-C,... stretching vibrations - and thus allows no definite determination of the “real” physical structure and chemical composition of the grain particles. Therefore, observational conclusions concerning the properties of circumstellar dust can provide only some “mean” information which allows no definitive conclusions regarding the true nature of the observed grains (geometrical shape, crystalline structure,...?).

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 167 - 173
Copyright
Copyright © Springer-Verlag 1988

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