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

M. Farzone; N. Ryde; G.M. Harper; J. Lambert; E. Josselin; M. J. Richter; K. Eriksson

doi:10.1051/eas/1360017

All issues

Volume 60 (2013)

EAS Publications Series, 60 (2013) 155-159

Abstract

Issue		EAS Publications Series Volume 60, 2013 Betelgeuse Workshop 2012 The Physics of Red Supergiants: Recent Advances and Open Questions


Page(s)		155 - 159
Section		Atmospheric Structure and Dynamics
DOI		https://doi.org/10.1051/eas/1360017
Published online		23 May 2013

Betelgeuse Workshop 2012
P. Kervella, T. Le Bertre and G. Perrin (eds)
EAS Publications Series, 60 (2013) 155-159

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

M. Farzone¹, N. Ryde¹, G.M. Harper², J. Lambert¹^,3, E. Josselin³, M. J. Richter⁴ and K. Eriksson⁵

¹ Lund Observatory, Box 43, 221 20 Lund, Sweden
² School of Physics, Trinity College Dublin, College Green, Dublin 2, Ireland
³ LUPM, CNRS, Université Montpellier II, Pl. Bataillon, 34095 Montpellier Cedex, France
⁴ Department of Physics, University of California at Davis, One Shields Avenue, Davis, CA 95616, USA
⁵ Department of Physics & Astronomy, Box 516, 751 20 Uppsala, Sweden

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.