A new method for the spectroscopic identification of stellar non-radial pulsation modes

Free access article

This article is an erratum for: [this article]

Issue		A&A Volume 497, Number 3, April III 2009


Page(s)		827 - 827
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361/20064876e
Published online		09 February 2009

Erratum

I. The method and numerical tests

W. Zima

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 $\chi^2_\nu$ 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 $\ell$ and the non-adiabatic parameter f for non-radially pulsating stars.

I apologize for not mentioning this in the original paper.

References

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)

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