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Light curves of the Be stars of NGC 3766

Published online by Cambridge University Press:  12 July 2011

Rachael M. Roettenbacher  and
M. Virginia McSwain
Rachael M. Roettenbacher
Affiliation:
Lehigh University, Department of Physics, 16 Memorial Drive E, Bethlehem, PA, 18015, USA email: rmr207@lehigh.edu, mcswain@lehigh.edu
M. Virginia McSwain
Affiliation:
Lehigh University, Department of Physics, 16 Memorial Drive E, Bethlehem, PA, 18015, USA email: rmr207@lehigh.edu, mcswain@lehigh.edu
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Abstract

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Nonradial pulsations (NRPs) are a possible formation mechanism for the equatorial disks surrounding Be stars. The open cluster NGC 3766 has a high fraction of transient Be stars, Be stars that have been observed with both emission due to a circumstellar disk and a non-emitting B-type spectrum. Because of the large fraction of transient Be stars, this cluster is a prime location for studying the formation mechanisms of Be star disks. We observed NGC 3766 for more than 25 nights over three years to generate Strömgren uvby light curves of the Be population. We present the results of a period search to investigate the presence of NRPs.

Keywords

open clusters and associations: individual (NGC 3766)stars: emission-lineBestars: oscillations (including pulsations)
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. 545 - 546
Copyright
Copyright © International Astronomical Union 2011

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