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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: hwenjin@astro.washington.edu
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: gies@chara.gsu.edu
M. Virginia McSwain
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015; email: mcswain@lehigh.edu
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Abstract

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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

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