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Spectra of M Dwarfs - Dimmed by Dust

Published online by Cambridge University Press:  14 August 2015

T. Tsuji ,
K. Ohnaka ,
W. Aoki  and
H.R.A. Jones
T. Tsuji
Affiliation:
Institute of Astronomy, The University of Tokyo 2-21-1 Osama, Mitaka, Tokyo, 181 Japan
K. Ohnaka
Affiliation:
Institute of Astronomy, The University of Tokyo 2-21-1 Osama, Mitaka, Tokyo, 181 Japan
W. Aoki
Affiliation:
Institute of Astronomy, The University of Tokyo 2-21-1 Osama, Mitaka, Tokyo, 181 Japan
H.R.A. Jones
Affiliation:
Institute of Astronomy, The University of Tokyo 2-21-1 Osama, Mitaka, Tokyo, 181 Japan

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Spectra of M dwarfs are rich in atomic and molecular lines. These spectra provide such basicinformation as Teff (or radius), log g (or mass), surface chemical composition, and something more (e.g. activity) if properly interpreted. It is recognized, however, that spectra of M dwarfs are already dimmed by the dust formed in their photospheres (Tsuji et al. 1996a) and this effect, which has been overlooked until recently, should be taken into account in any interpretation and analysis of the spectra of very low mass objects (VLMOs) including late M dwarfs and brown dwarfs.

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