SIMBAD references

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 (2.0-2.4µm) and L (3.4-4.1µm) 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 µm 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 11µm); 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 11µm 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 11µm); 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 11µm there was no data available. For R Leonis the model dust shell has a moderate optical depth (0.1 at 11µm); in K and L the visibility data and model situation is similar to that of SW Vir, and at 11µm 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 11µm, 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.