Volume 505, Number 2, October II 2009
|Page(s)||687 - 693|
|Section||Interstellar and circumstellar matter|
|Published online||11 August 2009|
VLTI/MIDI observations of 7 classical Be stars*
Max Planck Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany e-mail: firstname.lastname@example.org
2 UMR 6525 CNRS FIZEAU UNS, OCA, CNRS, Campus Valrose, 06108 Nice Cedex 2, France
3 Physics and Astronomy Department, The University of Western Ontario, London, N6A 3K7, Ontario, Canada
Accepted: 1 August 2009
Context. 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.
Aims. 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.
Methods. 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 130 m to obtain an angular resolution of about 15 mas in the N band and compared our results with previous K band measurements obtained with the VLTI/AMBER instrument and/or the CHARA interferometer.
Results. 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 130 m, evidence that their circumstellar disk extension is less than 10 mas. The only exception is α Ara, which is clearly resolved and well-fitted by an elliptical envelope with a major axis mas and an axis ratio at 8 μm. This extension is similar to the size and flattening measured with the VLTI/AMBER instrument in the K band at 2 μm.
Conclusions. The size of the circumstellar envelopes for these classical Be stars does not seem to vary strongly on the observed wavelength between 8 and 12 μm. Moreover, the size and shape of α Ara's disk is almost identical at 2, 8, and 12 μm. 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.
Key words: techniques: high angular resolution / techniques: interferometric / stars: emission-line, Be / stars: winds, outflows / stars: general / stars: circumstellar matter
© ESO, 2009
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