In the original article, there was a mistake in Figure 3 as published.
Figure 3
This figure aimed at exploring trends regarding the contribution from the dominant model properties (i.e., mass, initial metal mass fraction, and overshoot parameter) toward the convective core sizes of the best-fit models of α Centauri A. However, the data plotted in Figure 3 in the original article represents the models with convective cores that satisfy a probability threshold required to fit the sets of observables (i.e., seismic observables, classical observables, and an interferometric radius), instead of showing the best-fit models with convective cores that satisfy the sets of observables within 1σ. The corrected Figure 3 appears below.
The authors apologize for this error and state that this does not change the scientific conclusions of the article in any way. The original article has been updated.
Summary
Keywords
HD 128620, asteroseismology, stellar modeling, fundamental parameters, convection, radiation
Citation
Nsamba B, Campante TL, Monteiro MJPFG, Cunha MS and Sousa SG (2019) Corrigendum: On the Nature of the Core of α Centauri A: The Impact of the Metallicity Mixture. Front. Astron. Space Sci. 6:67. doi: 10.3389/fspas.2019.00067
Received
02 July 2019
Accepted
04 October 2019
Published
25 October 2019
Volume
6 - 2019
Edited by
Jadwiga Daszynska-Daszkiewicz, University of Wrocław, Poland
Reviewed by
Joyce Ann Guzik, Los Alamos National Laboratory (DOE), United States
Updates
Copyright
© 2019 Nsamba, Campante, Monteiro, Cunha and Sousa.
This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
*Correspondence: Benard Nsamba benard.nsamba@astro.up.pt
This article was submitted to Stellar and Solar Physics, a section of the journal Frontiers in Astronomy and Space Sciences
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