Abstract
Context. Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar disk that is responsible for the observed IR-excess and emission lines. The influence of binarity on these phenomena remains controversial.
Highlights
Classical Be stars are close-to-main-sequence hot stars that show or have shown infrared excess and emission lines in their spectra
Considering that they are fast rotators, a generally accepted view of these objects is that their circumstellar environment consists of two distinct regions: a dense equatorial disk dominated by rotation where most of the infrared radiation and emission lines are produced and a more diluted polar wind responsible for the highly broadened ultraviolet lines
We discovered that two other K-band emission lines were strong enough to support the kinematics study: the He i line located at 2.06 μm, and the Brδ line around 1.94 μm
Summary
A. Meilland1, O. Delaa2, Ph. Stee2, S. Kanaan3, F. Millour2, D. Mourard2, D. Bonneau2, R. Petrov2, N. Nardetto2, A. Marcotto2, A. Roussel2, J. M. Clausse2, K. Perraut4, H. McAlister5,6, T. ten Brummelaar6, J. Sturmann6, L. Sturmann6, N. Turner6, S. T. Ridgway7, C. Farrington6, and P. J. Goldfinger6
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