Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-05T19:29:05.905Z Has data issue: false hasContentIssue false
  • English
  • Français

Results from a recent stellar rotation census of B stars

Published online by Cambridge University Press:  12 July 2011

Wenjin Huang ,
Douglas R. Gies  and
M. Virginia McSwain
Wenjin Huang
Affiliation:
Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 email: [email protected]
Douglas R. Gies
Affiliation:
Center for High Angular Resolution Astronomy, Department of Physics and Astronomy Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106; email: [email protected]
M. Virginia McSwain
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015; email: [email protected]
Rights & Permissions [Opens in a new window]

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.

In an analysis of the rotational properties of more than 1100 B stars (~660 cluster and ~500 field B stars), we determine the projected rotational velocity (V sin i), effective temperature, gravity, mass, and critical rotation speed for each star. The new data provide us a solid observational base to explore many hot topics in this area: Why do field B stars rotate slower than cluster B stars? How fast do B stars rotate when they are just born? How fast can B stars rotate before they become Be stars? How does the rotation rate of B stars change with time? Does the evolutionary change in rotation velocity lead to the Be phenomenon? Here we report the results of our efforts in searching for answers to these questions based on the latest B star census.

Keywords

line: profilesstars: early-typestars: emission-lineBestars: fundamental parametersstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 89 - 90
Copyright
Copyright © International Astronomical Union 2011

References

Abt, H. A., Levato, H., & Grosso, M. 2002, ApJ, 573, 359CrossRefGoogle Scholar
Ekström, S., Meynet, G., Maeder, A., & Barblan, F. 2008, A&A, 478, 467Google Scholar
Heger, A. & Langer, N. 2000, ApJ, 544, 1016CrossRefGoogle Scholar
Huang, W. & Gies, D. R. 2006a, ApJ, 648, 580CrossRefGoogle Scholar
Huang, W. & Gies, D. R. 2006b, ApJ, 648, 591CrossRefGoogle Scholar
Huang, W., Gies, D. R., & McSwain, M. V. 2010, ApJ 722, 605CrossRefGoogle Scholar
Meynet, G. & Maeder, A. 2000, A&A, 361, 101Google Scholar
Wolff, S. C., Strom, S. E., Dror, D., & Venn, K. 2007, AJ, 133, 1092CrossRefGoogle Scholar