Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-12-01T11:44:55.306Z Has data issue: false hasContentIssue false
  • English
  • Français

Shell Lines in Be Disks

Published online by Cambridge University Press:  12 April 2016

R. W. Hanuschik
R. W. Hanuschik*
Affiliation:
Data Management and Operations Division, European Southern Observatory, D-85748 Garching, Germany

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Shell lines have high diagnostic potential for the kinematical conditions in Be disks. We present here results from our long-term spectroscopic monitoring campaign of Fe II shell lines. We demonstrate that most of them are likely to arise in Keplerian disks being hydrostatically supported. There is furthermore one class of shell lines (dubbed NOACs) which does not fit into this simple scheme.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 518 - 522
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Bjorkman, J.E., Cassinelli, J.P. 1993, ApJ 409, 429 Google Scholar
Hanuschik, R.W. 1995, A&A 295, 423 Google Scholar
Hanuschik, R.W., Hummel, W., Dietle, O., Sutorius, E. 1995, A&A 300, 163 Google Scholar
Hanuschik, R.W., Vrancken, M., 1996, A&A 312, L17 Google Scholar
Hanuschik, R.W., Hummel, W., Sutorius, E., Dietle, O., Thimm, G. 1996, A&AS 116, 309 Google Scholar
Rivinius, Th., Štefl, S., Baade, D. 1999, A&A, in pressGoogle Scholar