Issue |
A&A
Volume 389, Number 1, July I 2002
|
|
---|---|---|
Page(s) | 345 - 354 | |
Section | Numerical methods and codes | |
DOI | https://doi.org/10.1051/0004-6361:20020549 | |
Published online | 14 June 2002 |
Abundance analysis of targets for the COROT/MONS asteroseismology missions*
I. Semi-automatic abundance analysis of the γ Dor star HD 49434
1
Institute for Physics and Astronomy, University of Aarhus, Bygn. 520, 8000 Aarhus C, Denmark
2
Laboratoire d'Astrophysique de l'OMP, CNRS UMR 5572, Observatoire Midi-Pyrénées, 14 avenue Édouard Belin, 31400 Toulouse, France
3
Laboratoire d'Astrophysique de Marseille, France
4
Instituto de Astrofísica de Andaluciá, Spain
5
Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria
6
Observatoire de Paris, France
Corresponding author: H. Bruntt, bruntt@ifa.au.dk
Received:
23
January
2002
Accepted:
5
April
2002
One of the goals of the ground-based
support program for the COROT and MONS/Rømer satellite missions
is to select and characterise suitable target stars for the
part of the missions dedicated to asteroseismology.
While the global atmospheric parameters may be determined
with good accuracy from the Strömgren indices, careful
abundance analysis must be made for the proposed main targets.
This is a time consuming process considering
the long list of primary and secondary targets.
We have therefore developed new software called vwa for this task.
The vwa automatically selects
the least blended lines from the atomic line database vald, and
consequently adjusts the abundance in order to find the best match
between the calculated and observed spectra.
The variability of HD 49434 was discovered as part of COROT
ground-based support observations. Here
we present a detailed abundance analysis of HD 49434 using vwa.
For most elements we find abundances somewhat below
the Solar values, in particular we find [Fe/H] .
We also present the results from the study of the variability
that is seen in spectroscopic and photometric time series
observations.
From the characteristics of the variation seen in photometry and
in the line profiles we propose that HD 49434 is a variable star
of the γ Doradus type.
Key words: methods: data analysis / techniques: spectroscopic / stars: abundances / stars: fundamental parameters / stars: individual: HD 49434
© ESO, 2002
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