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Limits for the application of spectroscopic mode ID methods

Published online by Cambridge University Press:  02 March 2005

W. Zima ,
K. Kolenberg ,
M. Briquet  and
M. Breger
W. Zima
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria e-mail: [email protected]
K. Kolenberg
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria e-mail: [email protected] Instituut voor Sterrenkunde, Celestijnenlaan 200B, 3001 Heverlee, Belgium
M. Briquet
Affiliation:
Instituut voor Sterrenkunde, Celestijnenlaan 200B, 3001 Heverlee, Belgium
M. Breger
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria e-mail: [email protected]
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Abstract

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Spectroscopic mode identification techiques, which monitor intensity variations across an absorption line, provide the possibility of determining the quantum numbers l and m, the inclination and the intrinsic pulsation amplitude of a star. Of course, the uncertainties of the mode identification are dependent on the quality of the observations and the identification method applied. We have focused on the Pixel-by-pixel method/Direct line profile fitting (Mantegazza 2000) and the Moment method (Balona 1987, Briquet & Aerts 2003) for pinpointing mode parameters and tested the impact of various observational effects and stellar properties on the identification.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Line: profilesmethods: numericaltechniques: spectroscopicstars: individual: (FG Vir, 44 Tau)stars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 780 - 785
Copyright
© 2004 International Astronomical Union