Hostname: page-component-586b7cd67f-t7czq Total loading time: 0 Render date: 2024-11-25T18:52:15.465Z Has data issue: false hasContentIssue false
  • English
  • Français

How Frequent is Evolutionary Spin-Up in Binary Be Stars?

Published online by Cambridge University Press:  26 May 2016

M. Maintz ,
Th. Rivinius ,
S. Štefl  and
O. Stahl
M. Maintz
Affiliation:
Landessternwarte Königstuhl, D-69117 Heidelberg, Germany
Th. Rivinius
Affiliation:
Landessternwarte Königstuhl, D-69117 Heidelberg, Germany ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
S. Štefl
Affiliation:
Astronomical Institute, Academy of Sciences, CZ-251 65 Ondřejov, Czech Republic
O. Stahl
Affiliation:
Landessternwarte Königstuhl, D-69117 Heidelberg, 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.

Satellite absorptions are identified as a general feature of Be binaries. In addition, Be + sdO binaries seem to show a characteristic short-term emission variability and short-lived shell events. The identification of such features can ease the search for further Be binaries with hot companions to allow an estimate of the fraction of Be Stars, possibly spun-up through binary evolution.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 95 - 96
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Gies, D.R., Bagnuolo, W.G. Jr., Ferrara, E.C. et al. 1998, ApJ 493, 440 Google Scholar
Hummel, W., Štefl, S. 2001, A&A 368, 471 Google Scholar
Peters, G. 1983, PASP 95, 311 Google Scholar
Poeckert, R. 1981, PASP 93, 297 CrossRefGoogle Scholar