Free access article

A&A 498, 127-138 (2009)
DOI: 10.1051/0004-6361/20079063

The dust condensation sequence in red supergiant stars

T. Verhoelst^{1, 2}, N. Van der Zypen¹, S. Hony³, L. Decin¹, J. Cami⁴, and K. Eriksson<sup>5

1</sup>  Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
    e-mail: tijl.verhoelst@ster.kuleuven.be
²  University of Manchester, Jodrell Bank Centre for Astrophysics, Manchester M13 9PL, UK
³  Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, DAPNIA/SAp, 91191 Gif-sur-Yvette, France
⁴  Physics and Astronomy Dept, University of Western Ontario, London ON N6A 3K7, Canada
⁵  Institute for Astronomy and Space Physics, Box 515, 75120 Uppsala, Sweden

Received 13 November 2007 / Accepted 31 December 2008

Abstract
Context. Red supergiant (RSG) stars exhibit significant mass loss by means of a slow, dense wind. They are often considered to be the more massive counterparts of Asymptotic Giant Branch (AGB) stars. While AGB mass loss is related to their strong pulsations, the RSG are often only weakly variable. This raises the question of whether their wind-driving mechanism and the dust composition of the wind are the same.
Aims. We study the conditions at the base of the wind by determining the dust composition of a sample of RSG. The dust composition is assumed to be sensitive to the density, temperature, and acceleration at the base of the wind. We compare the derived dust composition with the composition measured in AGB star winds.
Methods. We compile a sample of 27 RSG infrared spectra (ISO-SWS) and supplement these with photometric measurements to derive the full spectral energy distribution (SED). These data are modelled using a dust radiative-transfer code, taking into account the optical properties of the relevant candidate materials to search for correlations between mass-loss rate, density at the inner edge of the dust shell, and stellar parameters.
Results. We find strong correlations between the dust composition, mass-loss rate, and the stellar luminosity, roughly in agreement with the theoretical dust condensation sequence. We identify the need for a continuous (near-)IR dust opacity and tentatively propose amorphous carbon, and we note significant differences with AGB star winds in terms of the presence of PAHs, absence of “the” 13 m band, and a lack of strong water bands.
Conclusions. Dust condensation in RSG is found to experience a freeze-out process that is similar to that in AGB stars. Together with the positive effect of the stellar luminosity on the mass-loss rate, this suggests that radiation pressure on dust grains is an important ingredient in the driving mechanism. Still, differences with AGB stars are manifold and thus the winds of RSG should be studied individually in further detail.

Key words: techniques: spectroscopic -- stars: atmospheres -- circumstellar matter -- supergiants -- stars: mass-loss -- dust, extinction

© ESO 2009

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