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Nonradial pulsations in the open cluster NGC 3766

Published online by Cambridge University Press:  18 January 2010

Rachael M. Roettenbacher ,
Ernest C. Amouzou  and
M. Virginia McSwain
Rachael M. Roettenbacher
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive E, Bethlehem, PA, USA email: rmr207@lehigh.edu, eca2@lehigh.edu, mcswain]@lehigh.edu
Ernest C. Amouzou
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive E, Bethlehem, PA, USA email: rmr207@lehigh.edu, eca2@lehigh.edu, mcswain]@lehigh.edu
M. Virginia McSwain
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive E, Bethlehem, PA, USA email: rmr207@lehigh.edu, eca2@lehigh.edu, mcswain]@lehigh.edu
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Abstract

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Nonradial pulsations (NRPs) are a proposed mechanism for the formation of decretion disks around Be stars. They are important tools to study the internal structure of stars. NGC 3766 has an unusually large fraction of transient Be stars, so it is an excellent location to study the formation mechanism of Be-star disks. High-resolution spectroscopy can reveal line-profile variations from NRPs, allowing measurements of both the degree, l, and azimuthal order, m. However, spectroscopic studies require large amounts of time with large telescopes to achieve the necessary high signal-to-noise ratio and time-domain coverage. On the other hand, multicolor photometry can be performed more easily with small telescopes to measure l only. Here, we present representative light curves of Be stars and nonemitting B stars in NGC 3766 from the CTIO 0.9m telescope in an effort to study NRPs in this cluster.

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 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 518 - 521
Copyright
Copyright © International Astronomical Union 2010

References

Ahmed, F. 1962, Publ. Roy. Obs. Edinburgh, 3, 57Google Scholar
Balona, L. A. & Engelbrecht, C. A. 1986, MNRAS, 219, 131CrossRefGoogle Scholar
Buta, R. J. & Smith, M. A. 1979, ApJ, 232, 213CrossRefGoogle Scholar
De Ridder, J. 2001, PhD Thesis, Katholieke Univ. LeuvenGoogle Scholar
Gutiérrez–Soto, J., Fabregat, J., Suso, J., Lanzara, M., Garrido, R., Hubert, A.-M., & Floquet, M. 2007, A&A, 476, 927Google Scholar
McSwain, M. V., Huang, W., Gies, D. R., Grundstrom, E. D., & Townsend, R. H. D. 2008, ApJ, 672, 590CrossRefGoogle Scholar
Porter, J. M. & Rivinius, T. 2003, PASP, 115, 1153CrossRefGoogle Scholar
Rivinius, T., Baade, D., & Stefl, S. 2003, A&A, 411, 229Google Scholar