2009A&A...505..687M

Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar envelope that is responsible for the observed IR-excess and emission lines. The origin of this envelope, its geometry, and kinematics have been debated for some time. We measured the mid-infrared extension of the gaseous disk surrounding seven of the closest Be stars in order to constrain the geometry of their circumstellar environments and to try to infer physical parameters characterizing these disks. Long baseline interferometry is the only technique that enables spatial resolution of the circumstellar environment of classical Be stars. We used the VLTI/MIDI instrument with baselines up to 130m to obtain an angular resolution of about 15mas in the N band and compared our results with previous K band measurements obtained with the VLTI/AMBER instrument and/or the CHARA interferometer. We obtained one calibrated visibility measurement for each of the four stars, p Car, ζ Tau, κ CMa, and α Col, two for δ Cen and β CMi, and three for α Ara. Almost all targets remain unresolved even with the largest VLTI baseline of 130m, evidence that their circumstellar disk extension is less than 10mas. The only exception is α Ara, which is clearly resolved and well-fitted by an elliptical envelope with a major axis a=5.8±0.8mas and an axis ratio a/b=2.4±1 at 8µm. This extension is similar to the size and flattening measured with the VLTI/AMBER instrument in the K band at 2µm. The size of the circumstellar envelopes for these classical Be stars does not seem to vary strongly on the observed wavelength between 8 and 12µm. Moreover, the size and shape of α Ara's disk is almost identical at 2, 8, and 12µm. We expected that longer wavelengths probe cooler regions and correspondingly larger envelopes, but this is clearly not the case from these measurements. For α Ara this could come from to disk truncation by a small companion; however, other explanations are needed for the other targets.