Volume 497, Number 3, April III 2009
|Page(s)||827 - 827|
|Section||Stellar structure and evolution|
|Published online||09 February 2009|
A new method for the spectroscopic identification of stellar non-radial pulsation modes
I. The method and numerical tests
Instituut voor Sterrenkunde, Celestijnenlaan 200D, 3001 Leuven, Belgium
A&A 455, 227-234 (2006), DOI: 10.1051/0004-6361:20064876
Key words: line: profiles - techniques: spectroscopic - stars: variables: general - errata, addenda
The formulae for in Eq. (1) and for the errors in Eqs. (2) and (3) were defined and proposed by Daszynska-Daszkiewicz (private communication). A similar definition, but for complex amplitudes of photometric and radial velocity variations, has already been applied by Daszynska-Daszkiewicz et al. (2003, 2005) in their method of simultaneous determination of the degree and the non-adiabatic parameter f for non-radially pulsating stars.
I apologize for not mentioning this in the original paper.
- Zima, W. 2006, A&A, 455, 227 [NASA ADS] [CrossRef] [EDP Sciences]
- Daszynska-Daszkiewicz, J., Dziembowski, W. A., & Pamyatnykh, A. A. 2003, A&A, 407, 999 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Daszynska-Daszkiewicz, J., Dziembowski, W. A., & Pamyatnykh, A. A. 2005, A&A, 441, 641 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
Copyright ESO 2009
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