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Opacity Problems in Cool Low Mass Stars

Published online by Cambridge University Press:  12 April 2016

Michael Scholz  and
Rainer Wehrse
Michael Scholz
Affiliation:
Institut f. Theoret. Astrophysik der Universität Heidelberg, Im Neuenheimer Feld 561, D-69120 Heidelberg, Germany
Rainer Wehrse
Affiliation:
Institut f. Theoret. Astrophysik der Universität Heidelberg, Im Neuenheimer Feld 561, D-69120 Heidelberg, Germany

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In this contribution we want to discuss M star atmospheres and their dependence on molecular opacities. A star belongs to the spectral class M if its optical and infrared spectrum shows strong bands of TiO and numerous strong metal lines so that for wavelengths < 4000 Å there is “hardly any flux left” (Jaschek & Jaschek 1987). M stars cover a very large range in luminosity: M dwarfs are the intrinsically faintest stars, whereas M giants and supergiants reach luminosities that are among the highest known. General properties of these objects are given in Table 1 (after Schmidt-Kaler 1982).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 146: Molecules in the Stellar Environment , 1994 , pp. 49 - 60
Copyright
Copyright © Springer-Verlag 1994

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