| Issue |
A&A
Volume 661, May 2022
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202140536e | |
| Published online | 16 May 2022 | |
A discontinuity in the luminosity–mass relation and fluctuations in the evolutionary tracks of low-mass and low-metallicity stars at the Gaia M-dwarf gap (Corrigendum)
1
Helmholtz-Institut für Strahlen- und Kernphysik (HISKP), Universität Bonn, Nußallee 14-16, 53115 Bonn, Germany
e-mail: smansfield@astro.uni-bonn.de
2
Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovičkách 2, 18000 Praha, Czech Republic
Key words: stars: low-mass / convection / Hertzsprung-Russell and C-M diagrams / stars: luminosity function, mass function / errata, addenda
The initial helium abundance used in the models was Y = 0.28 and not the stated metallicity-dependent value of Y = 0.24 + 2Z. The mass ranges for models that undergo the convective kissing instability with this initial helium abundance are: 0.33000 M⊙ ≤ m ≤ 0.37100 M⊙ for Z = 0.01, 0.34300 M⊙ ≤ m ≤ 0.36900 M⊙ for Z = 0.001, and 0.35600 M⊙ ≤ m ≤ 0.39033 M⊙ for Z = 0.0001. All conclusions remain accurate except that the instability here occurs at a higher mass range for lower metallicity.
© S. Mansfield and P. Kroupa 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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