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What is the Origin of the Water Vapour Signatures in Red Giant Stars?

Published online by Cambridge University Press:  23 May 2013

M. Farzone ,
N. Ryde ,
G.M. Harper ,
J. Lambert ,
E. Josselin ,
M. J. Richter  and
K. Eriksson
M. Farzone
Affiliation:
Lund Observatory, Box 43, 221 20 Lund, Sweden
N. Ryde
Affiliation:
Lund Observatory, Box 43, 221 20 Lund, Sweden
G.M. Harper
Affiliation:
School of Physics, Trinity College Dublin, College Green, Dublin 2, Ireland
J. Lambert
Affiliation:
Lund Observatory, Box 43, 221 20 Lund, Sweden LUPM, CNRS, Université Montpellier II, Pl. Bataillon, 34095 Montpellier Cedex, France
E. Josselin
Affiliation:
LUPM, CNRS, Université Montpellier II, Pl. Bataillon, 34095 Montpellier Cedex, France
M. J. Richter
Affiliation:
Department of Physics, University of California at Davis, One Shields Avenue, Davis, CA 95616, USA
K. Eriksson
Affiliation:
Department of Physics & Astronomy, Box 516, 751 20 Uppsala, Sweden
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Abstract

We investigate the occurrence of water vapour signatures in a total of 10 red giants in the solar neighbourhood at mid-infrared wavelengths (12 μm). With the use of high resolution spectra from TEXES and synthesized spectra based on MARCS model atmospheres, we analyse the differences and discuss plausible causes. These include abundance adjustments, the addition of non-photospheric components (MOLspheres) and a different temperature profile.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 60: Betelgeuse Workshop 2012 The Physics of Red Supergiants: Recent Advances and Open Questions , 2013 , pp. 155 - 159
Copyright
© EAS, EDP Sciences 2013

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