Molecular and Dust Features in mass-losing AGB Stars, Models and ISO-Observations
- Author(s)
- Bernhard Aringer, Franz Kerschbaum, Susanne Höfner, Uffe Grae Jorgensen, R. Loidl, W Windsteig
- Abstract
Until recently, synthetic spectra for AGB stars have usually been calculated by using hydrostatic model atmospheres like the MARCS code. This is problematical, since AGB stars are dominated by dynamical phenomena like pulsation, shock waves, dust formation, and heavy mass loss. As a consequence, classical hydrostatic models fail to reproduce the observed intensities and variations of molecular features. To address these problems, we have computed synthetic spectra based on dynamical atmospheres from Höfner et al. (1998; these proceedings) by calculating chemical abundances of molecular species, continuum absorption, and molecular opacities for a given temperature-pressure structure (COMA code). For carbon stars we can also include dust opacities. The results are then taken as input for a radiative transfer code.
- Organisation(s)
- Department of Astrophysics
- External organisation(s)
- Uppsala University
- Pages
- 307
- Publication date
- 1998
- Austrian Fields of Science 2012
- 103003 Astronomy, 103004 Astrophysics
- Portal url
- https://ucrisportal.univie.ac.at/en/publications/molecular-and-dust-features-in-masslosing-agb-stars-models-and-isoobservations(696ad198-55cc-4d53-a5cb-b565a958af8b).html