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

¹ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
² Harvard-Smithsonian Center for Astrophysics, MS-20, 60 Garden Street, Cambridge, MA 02138, USA
³ Observatoire de Paris, LERMA, 61 avenue de l'Observatoire, 75014 Paris, France
⁴ Observatoire de Paris, LESIA, 5 place Jules Janssen, 92195 Meudon, France
⁵ Jet Propulsion Laboratory, MS 306-388, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
⁶ Observatoire de la Côte d'Azur, Département Fresnel UMR 6528, BP 4229, 06304 Nice, France
⁷ National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726, USA

Corresponding author: P. Schuller, pschuller@cfa.harvard.edu

Received: 13 March 2003
Accepted: 15 January 2004

Abstract

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 () and L () bands. Aiming at an explanation of these findings, we chose the objects α 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 interferometric data were also taken into account to further constrain the models. – We find the following results. For all three AGB stars, the photosphere and dust shell model is consistent with the multi-wavelength photometric data. For α Orionis the model dust shell has a very small optical depth (0.0065 at ); the visibility data and model in K and L are essentially entirely photospheric with no significant contribution from the dust, and the visibility data at show a strong dust signature which agrees with the model. For SW Virginis the model dust shell has a small optical depth (0.045 at ); in K the visibility data and model are essentially purely photospheric, in L the visibility data demand a larger object than the photosphere plus dust model allows, and at there was no data available. For R Leonis the model dust shell has a moderate optical depth (0.1 at ); in K and L the visibility data and model situation is similar to that of SW Vir, and at the visibility data and model are in agreement. – We conclude that AGB models comprising a photosphere and dust shell, although consistent with SED data and also interferometric data in K and at , 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.