Reference : The photospheric abundances of active binaries. III. Abundance peculiarities at high ...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/31888
The photospheric abundances of active binaries. III. Abundance peculiarities at high activity levels
English
Morel, Thierry [Osservatorio Astronomico di Palermo G. S. Vaiana, Istituto Nazionale di Astrofisica > > > >]
Micela, G. [Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Palermo G. S. Vaiana, Piazza del Parlamento 1, 90134 Palermo, Italy]
Favata, F. [Astrophysics Division - Research and Science Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands]
Katz, D. [Observatoire de Paris, GEPI, Place Jules Janssen, 92195 Meudon, France]
1-Nov-2004
Astronomy and Astrophysics
EDP Sciences
426
1007-1020
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] stars: fundamental parameters ; stars: abundances ; stars: activity ; line: formation
[en] We report the determination from high-resolution spectra of the atmospheric parameters and abundances of 13 chemical species (among which lithium) in 8 single-lined active binaries. These data are combined with our previous results for 6 other RS CVn systems to examine a possible relationship between the photospheric abundance patterns and the stellar activity level. The stars analyzed are generally found to exhibit peculiar abundance ratios compared to inactive, Galactic disk stars of similar metallicities. We argue that this behaviour is unlikely to be an artefact of errors in the determination of the atmospheric parameters or non-standard mixing processes along the red giant branch, but diagnoses instead the combined action of various physical processes related to activity. The most promising candidates are cool spot groups covering a very substantial fraction of the stellar photosphere or NLTE effects arising from nonthermal excitation. However, we cannot exclude the possibility that more general shortcomings in our understanding of K-type stars (e.g. inadequacies in the atmospheric models) also play a significant role. Lastly, we call attention to the unreliability of the (V-R) and (V-I) colour indices as temperature indicators in chromospherically active stars. Based on observations collected at the European Southern Observatory, Chile (Proposals 64.L-0249 and 071.D-0260). Table A.1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/426/1007
http://hdl.handle.net/2268/31888
10.1051/0004-6361:20041047
http://adsabs.harvard.edu/abs/2004A%26A...426.1007M
http://de.arxiv.org/abs/astro-ph/0406348

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