Issue |
A&A
Volume 538, February 2012
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Article Number | A48 | |
Number of page(s) | 15 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/201117398 | |
Published online | 31 January 2012 |
Online material
Observed Fe i and Fe ii lines.
Other lines studied.
Appendix A: Supplementary material
A.1. GLMP 334 and IRAS 15482–5741
We provide an additional set of figures for both post-AGB stars in this section. We aim to shown the behavior of theoretical predictions by changing the AGB initial mass and 13C-pocket efficiency. The discrepancy between predicted and observed [C, N/Fe] may be improved by increasing the metallicity by 0.2 dex in both stars. This would reduce the predicted [C/Fe] by 0.3 dex with respect to Figs. 3 and 4, while leaving [ls/Fe] and [hs/Fe] unchanged. Indeed, 12C is primarily produced during partial He burning in the convective thermal pulse (independently of the metallicity) and is then dredged-up in the envelope after each TDU. In Figs. A.13 and A.14 we present two special cases modelled for both post-AGB stars. We present a summary of the theoretical interpretations of the two post-AGB stars discussed here compared with other post-AGB stars found in the literature in Sect. A.2.
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Fig. A.1
GLMP 334: the same as Fig. 3, but showing an additional 13C-pocket (case ST, thin solid line). This figure shows as by further decreasing the s-process efficiency, the observed [hs/Fe] is underestimated by the theoretical prediction. |
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Fig. A.2
GLMP 334: the same as Fig. 3, but for |
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Fig. A.3
GLMP 334: the same as Fig. A.2, but for |
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Fig. A.4
GLMP 334: the same as Fig. A.2, but for |
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Fig. A.5
GLMP 334: the same as Fig. A.2, but for |
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Fig. A.6
Theoretical interpretation of the post-AGB stars GLMP 334 ([Fe/H] = − 0.4; Teff = 7400 K; log g = 1.4) with |
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Fig. A.7
IRAS 15482–5741: the same as Fig. 4, but showing a different range of 13C-pockets: cases ST × 2 (solid line), ST (dotted thin line) and ST/3 (dotted thick line). This figure shows the behavior of the s-process elements if the 13C-pocket is changed. |
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Fig. A.8
IRAS 15482–5741: the same as Fig. 4, but for |
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Fig. A.9
IRAS 15482–5741: the same as Fig. 4, but for |
Open with DEXTER |
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Fig. A.10
IRAS 15482–5741: the same as Fig. A.9, but for |
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Fig. A.11
IRAS 15482–5741: the same as Fig. A.9, but for |
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Fig. A.12
Theoretical interpretation of the post-AGB star IRAS 15482–5741 ([Fe/H] = − 0.5; Teff = 7400 K; log g = 1.1) with |
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Fig. A.13
Theoretical interpretation of the post-AGB star GLMP 334 ([Fe/H] = − 0.4; Teff = 7400 K; log g = 1.4) by assuming a metallicity 0.2 dex higher than that observed. AGB models of initial mass of 1.5 M⊙ (19 TDUs), cases ST × 2 (solid line), ST × 1.7 (dotted thin line) and ST × 1.3 (dotted thick line) are shown. Note that the mass of the pocket was multiplied by a plausible factor of two to obtain 0.2 dex higher abundances in both [ls/Fe] and [hs/Fe]. We modelled these special cases to decrease [C/Fe] predictions with respect to Fig. 3, leaving [ls/Fe] and [hs/Fe] unchanged. |
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Fig. A.14
Theoretical interpretation of the post-AGB star IRAS 154825741 ([Fe/H] = − 0.5; Teff = 7400 K; log g = 1.1) by assuming a metallicity 0.2 dex higher than that observed. AGB models of initial mass of 1.4 M⊙ (10 TDU), cases ST × 2 (solid line), ST × 1.7 (dotted thin line) and ST × 1.3 (dotted thick line) are shown. Note that the mass of the pocket was multiplied by a plausible factor of two to obtain 0.2 dex higher abundances in both [ls/Fe] and [hs/Fe]. We modelled these special cases to decrease the [C/Fe] predictions with respect to Fig. 4, leaving [ls/Fe] and [hs/Fe] unchanged. |
Open with DEXTER |
A.2. Comparison with other post-AGB stars presented in the literature.
We provide in Table A.1 a summary of the theoretical interpretations of the post-AGB stars discussed in the literature. Solutions are found within the mass range = 1.4 to 3 M⊙. The choice of the 13C-pocket efficiency is peaked at ST/1.5, with a spread between ST/3 and ST × 2 (see also Gallino et al. 2008).
Summary of the stellar parameters, metallicities, [ls/Fe], [hs/Fe] and theoretical interpretations of the two post-AGB stars studied in this paper compared with the post-AGB stars discussed in the literature.
© ESO, 2012
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