Volume 570, October 2014
|Number of page(s)||1|
|Section||Stellar structure and evolution|
|Published online||07 October 2014|
Thermohaline instability and rotation-induced mixing (I, II, III) (Corrigendum)
School of Physics and Astronomy, Birmingham
152 TT Birmingham,
2 Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
3 IRAP, UMR 5277 CNRS and Université de Toulouse, 14, Av. E. Belin, 31400 Toulouse, France
4 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio, Italy
5 LUPM, Université Montpellier II, CNRS, UMR 5299, place E. Bataillon, 34095 Montpellier, France
Key words: asteroseismology / instabilities / stars: evolution / stars: interiors / stars: rotation / errata, addenda
Z = 0.0001.
Z = 0.002.
The initial rotation velocities of the stellar evolution models computed by Charbonnel & Lagarde (2010) and Lagarde et al. (2011, 2012) correspond to 30% instead of the published 45% of the critical velocity at the zero-age main sequence (ZAMS). An erroneous expression for the calculation of the critical velocity was used (cf. Sect. 2.3 of Lagarde et al. 2012). The correct expression for critical rotation velocity reads: (1)In Tables 1−4, we provide the assumed VZAMS as well as the corrected values of the ratio VZAMS/Vcrit for the published models at different metallicities.
We note that the model predictions are not further affected by this error, since all computations are made using the current velocity in [km s-1], not in units of critical velocity.
Z = 0.004.
Z = 0.014.
- Charbonnel, C., & Lagarde, N. 2010, A&A, 522, A10 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [PubMed] [Google Scholar]
- Lagarde, N., Charbonnel, C., Decressin, T., & Hagelberg, J. 2011, A&A, 536, A28 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Lagarde, N., Decressin, T., Charbonnel, C., et al. 2012, A&A, 543, A108 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO, 2014
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