| Issue |
A&A
Volume 546, October 2012
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/200912084e | |
| Published online | 01 October 2012 | |
Dust driven mass loss from carbon stars as a function of stellar parameters
I. A grid of solar-metallicity wind models (Corrigendum)
1
Dark Cosmology Centre, Niels Bohr Institute, University of
Copenhagen,
Juliane Maries Vej 30, 2100,
Copenhagen Ø,
Denmark
e-mail: mattsson@dark-cosmology.dk
2
Dept. of Physics and Astronomy, Div. of Astronomy and Space
Physics, Uppsala University, Box
515, 75120
Uppsala,
Sweden
Aims. The purpose of this corrigendum is to point out that a handful of models in the original paper were computed with faulty initial structures.
Methods. Using exactly the same modelling methods we have recomputed the faulty models with new initial structures.
Results. The new results slightly changes some of the trends in the wind properties with stellar parameters, but the overall effects are small. The conclusions are not affected
Key words: stars: AGB and post-AGB / stars: atmospheres / stars: carbon / circumstellar matter / stars: evolution / errata, addenda
© ESO, 2012
While recomputing parts of the grid of wind models (Mattsson et al. 2010) in order to obtain extended time sequences for modeling of spectral variation (Eriksson et al., in prep.) we discovered that a few models had faulty starting structures. A closer analysis revealed there were in total nine models that needed revision. We recomputed the faulty hydrostatic start models as well as the wind models and below we present a table (Table 1) with the resultant wind properties. Qualitatively, these
Input parameters (Δvp, M ⋆ , log (L ⋆ ), L ⋆ , Teff, log(C-O), P) and the resulting average mass loss rate, average wind speed and the mean degree of dust condensation at the outer boundary.
new numbers have no major impact on the overall result, although they would slightly affect the appearance of Figs. 6 and 7. The conclusions are not affected.
References
- Höfner, S., & Dorfi, E. A. 1997, A&A, 319, 648 [NASA ADS] [Google Scholar]
- Mattsson, L., Wahlin, R., & Höfner, S. 2010, A&A, 509, A14 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
All Tables
Input parameters (Δvp, M ⋆ , log (L ⋆ ), L ⋆ , Teff, log(C-O), P) and the resulting average mass loss rate, average wind speed and the mean degree of dust condensation at the outer boundary.
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