| Issue |
A&A
Volume 671, March 2023
|
|
|---|---|---|
| Article Number | C8 | |
| Number of page(s) | 1 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202038891e | |
| Published online | 10 March 2023 | |
Low-mass low-metallicity AGB stars as an efficient i-process site explaining CEMP-rs stars (Corrigendum)
1
Department of Physics, University of Calicut, Thenhipalam, Malappuram 673635, India
e-mail: drisyadev@gmail.com
2
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, ULB, Campus Plaine C.P. 226, Boulevard du Triomphe, 1050 Bruxelles, Belgium
3
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
4
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
5
Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
Key words: nuclear reactions / nucleosynthesis / abundances / stars: AGB and post-AGB / binaries: spectroscopic / stars: fundamental parameters / errata, addenda
We noticed a typo in Eq. (6), Sect. 7.2 of the original paper: the normalizing factor 1/N was erroneously omitted, though it was included when computing the reduced χ2 listed in Table 1. The correct equation is the following:
![$$ \begin{aligned} \chi ^2= \frac{1}{N} \sum _X \frac{\left({[\mathrm X/Fe]_{obs}}-{[\mathrm X/Fe]_{mod}}\right)^2}{\sigma ^2_{\rm X,obs}}\quad , \end{aligned} $$](/articles/aa/full_html/2023/03/aa38891e-20/aa38891e-20-eq1.gif)
where [X/Fe]obs and [X/Fe]mod are the measured and predicted abundances of a given element X, respectively, and σX, obs is the associated uncertainty on the measured abundance; the number of considered elements is N.
© The Authors 2023
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