| Issue |
A&A
Volume 689, September 2024
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/202451799e | |
| Published online | 30 August 2024 | |
Simulating small-scale dynamo action in cool main-sequence stars (Corrigendum)
1
Istituto ricerche solari Aldo e Cele Daccò (IRSOL), Faculty of Informatics, Università della Svizzera italiana,
6605
Locarno,
Switzerland
2
Euler Institute, Università della Svizzera italiana (USI),
6900
Lugano,
Switzerland
3
Leibniz-Institut für Sonnenphysik (KIS),
Schöneckstrasse 6,
79104
Freiburg i.Br.,
Germany
4
Theoretical Astrophysics, Department of Physics and Astronomy, Uppsala University,
Box 516,
751 20
Uppsala,
Sweden
Key words: dynamo / magnetohydrodynamics (MHD) / turbulence / methods: numerical / stars: atmospheres / errata, addenda
The x-axis of Fig. A.1 is erroneously multiplied by a factor of 1/3600. The correct x-axis is given in Fig. 1 below. None of the results or conclusions of the paper are affected by this correction. We apologize for any inconvenience that may have been caused by this mistake.
© The Authors 2024
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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All Figures
 |
Fig. 1 Temporal profiles of magnetic-to-kinetic energy ratios averaged over the convection zone, with the time coordinate normalized to the estimated turnover times of the four models. |
| In the text | |
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