Free access article

Issue A&A Volume 460, Number 2, December III 2006 Page(s) L9 - L12 Section Letters DOI 10.1051/0004-6361:20066322

A&A 460, L9-L12 (2006)
DOI: 10.1051/0004-6361:20066322

Letter

Too little radiation pressure on dust in the winds of oxygen-rich AGB stars

P. Woitke

Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
    e-mail: woitke@strw.leidenuniv.nl

(Received 30 August 2006 / Accepted 6 October 2006)

Abstract
Aims.It is commonly assumed that the massive winds of AGB stars are dust-driven and pulsation-enhanced. However, detailed frequency-dependent dynamical models that can explain the observed magnitudes of mass loss rates and outflow velocities have been published so far only for C-stars. This letter reports on first results of similar models for oxygen-rich AGB stars. The aim is to provide a better understanding of the wind driving mechanism, the dust condensation sequence, and the role of pulsations.
Methods.New dynamical models for dust-driven winds of oxygen-rich AGB stars are presented which include frequency-dependent Monte Carlo radiative transfer by means of a sparse opacity distribution technique and a time-dependent treatment of the nucleation, growth and evaporation of inhomogeneous dust grains composed of a mixture of Mg₂SiO₄, SiO₂, Al₂O₃, TiO₂, and solid Fe.
Results.The frequency-dependent treatment of radiative transfer reveals that the gas is cold close to the star ( K at ) which facilitates the nucleation process. The dust temperatures are strongly material-dependent, with differences as large as 1000 K for different pure materials, which has an important influence on the dust formation sequence. Two dust layers are formed in the dynamical models: almost pure glassy Al₂O₃ close to the star ( ) and the more opaque Fe-poor Mg-Fe-silicates further out. Solid Fe and Fe-rich silicates are found to be the only condensates that can efficiently absorb the stellar light in the near IR. Consequently, they play a key role in the wind driving mechanism and act as a thermostat. Only small amounts of Fe can be incorporated into the grains, because otherwise the grains become too hot. Thus, the models reveal almost no mass loss, and no dust shells.
Conclusions.The observed dust sequence Al₂O₃ Fe-poor Mg-Fe-silicates for oxygen-rich AGB stars having low high mass loss rates is in agreement with the presented model and can be understood as follows: Al₂O₃ is present in the extended atmosphere of the star below the wind acceleration region, also without mass loss. The Mg-Fe-silicates form further out and, therefore, their amount depends on the mass loss rate. The driving mechanism of oxygen-rich AGB stars is still an unsolved puzzle.

Key words: hydrodynamics -- radiative transfer -- stars: winds, outflows -- stars: mass-loss -- stars: AGB and post-AGB

© ESO 2006

What is OpenURL?