Volume 567, July 2014
|Number of page(s)||15|
|Published online||01 August 2014|
Abundance analysis for long-period variables
II. RGB and AGB stars in the globular cluster 47 Tucanae
1 University of Vienna, Department of Astrophysics, Türkenschanzstrasse 17, 1180 Vienna, Austria
2 National Optical Astronomy Observatory, 950 N.Cherry Avenue, Tucson, Arizona 85726, USA
3 Departement for Physics and Astronomy, Division of Astronomy and Space Physics, Uppsala University, Box 516, 75120 Uppsala, Sweden
Received: 28 April 2014
Accepted: 10 June 2014
Context. Asymptotic giant branch (AGB) stars play a key role in the enrichment of galaxies with heavy elements. Due to their large amplitude variability, the measurement of elemental abundances is a highly challenging task that has not been solved in a satisfactory way yet.
Aims. Following our previous work we use hydrostatic and dynamical model atmospheres to simulate observed high-resolution near-infrared spectra of 12 variable and non-variable red giants in the globular cluster 47 Tuc. The 47 Tuc red giants are independently well-characterized in important parameters (mass, metallicity, luminosity). The principal aim was to compare synthetic spectra based on the dynamical models with observational spectra of 47 Tuc variables. Assuming that the abundances are unchanged on the upper giant branch in these low-mass stars, our goal is to estimate the impact of atmospheric dynamics on the abundance determination.
Methods. To estimate abundances, we measured the equivalent widths of selected features in observed spectra and compared the results with predictions from a set of hydrostatic and dynamical model atmospheres resembling 47 Tuc AGB stars in their fundamental parameters. Our study includes lines of 12CO, 13CO, OH, and Na. Furthermore, we investigated the variations in line intensities over a pulsation cycle.
Results. We present new measurements of the C/O and 12C/13C ratio for 5 non-variable red giants in 47 Tuc. The equivalent widths measured for our 7 variable stars strongly differ from the non-variable stars and cannot be reproduced by either hydrostatic or dynamical model atmospheres. Nevertheless, the dynamical models fit the observed spectra of long-period variables much better than any hydrostatic model. For some spectral features, the variations in the line intensities predicted by dynamical models over a pulsation cycle give similar values as a sequence of hydrostatic models with varying temperature and constant surface gravity.
Conclusions. Our study of the dynamical effects on abundance determination visible in these well-characterized cluster stars prepares the ground for the long-term goal of deriving abundances for variable AGB stars in general.
Key words: stars: AGB and post-AGB / stars: late-type / stars: atmospheres / stars: abundances / line: profiles
© ESO, 2014
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