Abstract
We modeled the atmospheres of six carbon-rich Asymptotic Giant Branch stars (R Lep, R Vol, Y Pav, AQ Sgr, U Hya, and X TrA) using VLTI/MIDI interferometric observations, together with spectro-photometric data, we compared them with self-consistent, dynamic model atmospheres. The results show that the models can reproduce the Spectral Energy Distribution (SED) data well at wavelengths longer than 1 mu m, and the interferometric observations between 8 mu m and 10 mu m. We found differences at wavelengths shorter than 1 mu m in the SED, and longer than 10 mu m in the visibilities. The discrepancies observed can be explained in terms of a combination of data- and model-related reasons. We derived some stellar parameters, and our findings agree well with literature values within the uncertainties. Also, when comparing the location of the stars in the H-R diagram, with evolutionary tracks, the results show that the main derived properties (L, Teff, C/O ratios and stellar masses) from the model fitting are in good agreement with TP-AGB evolutionary calculations.
Originalsprache | Englisch |
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Seiten (von - bis) | 455-458 |
Seitenumfang | 4 |
Fachzeitschrift | Memorie Societa Astronomica Italiana |
Jahrgang | 88 |
Ausgabenummer | 3 |
Publikationsstatus | Veröffentlicht - Jan. 2017 |
ÖFOS 2012
- 103003 Astronomie
- 103004 Astrophysik