| Issue |
A&A
Volume 570, October 2014
|
|
|---|---|---|
| Article Number | C4 | |
| Number of page(s) | 2 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201424094e | |
| Published online | 03 November 2014 | |
KIC 10526294: a slowly rotating B star with rotationally split, quasi-equally spaced gravity modes (Corrigendum)⋆,⋆⋆
1 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
e-mail: Peter.Papics@ster.kuleuven.be
2 Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
3 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK
Key words: asteroseismology / stars: variables: general / stars: early-type / stars: fundamental parameters / stars: oscillations / stars: rotation / errata, addenda
Based on observations made with the William Herschel Telescope operated by the Isaac Newton Group on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.
Appendices are available in electronic form at http://www.aanda.org
An error occurred during the production process. An incorrect Fig. 12 was published. The correct Fig. 12 is published on the following page.
 |
Fig. 12
Five best fit models (from top to bottom, following the order in Table 6) using frequencies from MESA/GYRE. Upper panels: observed peaks (red circles, the error bars are smaller than the symbol size) versus the theoretical frequencies of the ℓ = 1 gravity modes (blue crosses, with the corresponding n value printed above). Lower panels: individual spacing values between the members of the observed period series (red filled circles) and the δp(p) function from the model (blue solid line). |
© ESO, 2014
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