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Global oscillations in Be star envelopes: observational evidence

Published online by Cambridge University Press:  26 May 2016

R. W. Hanuschik ,
W. Hummel ,
O. Dietle ,
J. Dachs  and
E. Sutorius
R. W. Hanuschik
Affiliation:
Astronomical Institute, University of Tübingen, D-72076 Tübingen, Germany
W. Hummel
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, Belgium
O. Dietle
Affiliation:
Astronomical Institute, Ruhr-Universität Bochum, D-44780 Bochum, Germany
J. Dachs
Affiliation:
Astronomical Institute, Ruhr-Universität Bochum, D-44780 Bochum, Germany
E. Sutorius
Affiliation:
Astronomical Institute, Ruhr-Universität Bochum, D-44780 Bochum, Germany

Extract

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Since 1982, we are performing a long-term spectroscopic observing programme of emission-lines in Be stars (Hanuschik 1987, Hanuschik et al. 1988, Dachs et al. 1992, Sutorius 1992, Dietle 1993). We are using ESO's 1.4m CAT, at resolution R ≥ 50 000 and S/N = 100–1000. Spectral lines chosen are the optically thick Hα, Hβ lines and the optically thin Fe ii λ5317 line. The latter line is an extremely sharp tracer (Δvth = 2 km s−1) for the kinematics in the disks. We believe that our atlas shows the full range of intrinsic structure of these emission lines.

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 384 - 385
Copyright
Copyright © Kluwer 1994 

References

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