Are dust shell models well-suited to explain interferometric data of late-type stars in the near-infrared?

Details Are dust shell models well-suited to explain interferometric data of late-type stars in the near-infrared? Are dust shell models well-suited to explain interferometric data of late-type stars in the near-infrared?

2004-01-22

arxiv.org/abs/astro-ph/0401479v1

Astron.Astrophys. 418 (2004) 151-162

Astronomy and Astrophysics

Astrophysics

12 pages, 4 figures, to be published in A&A; Latex aa class, uses packages graphicx, hyperref, natbib, and txfonts; keywords:

Scientific paper

10.1051/0004-6361:20040057

Recently available near-infrared interferometric data on late-type stars show a strong increase of diameter for asymptotic giant branch (AGB) stars between the K (2.0 - 2.4 \mu m) and L (3.4 - 4.1 \mu m) bands. Aiming at an explanation of these findings, we chose the objects \alpha Orionis (Betelgeuse), SW Virginis, and R Leonis, which are of different spectral types and stages of evolution, and which are surrounded by circumstellar envelopes with different optical thicknesses. For these stars, we compared observations with spherically symmetric dust shell models. Photometric and 11 \mu m interferometric data were also taken into account to further constrain the models. -- [...] -- We conclude that AGB models comprising a photosphere and dust shell, although consistent with SED data and also interferometric data in K and at 11 \mu m, cannot explain the visibility data in L; an additional source of model opacity, possibly related to a gas component, is needed in L to be consistent with the visibility data.

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