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Photometric variability of the Be star population with the KELT survey

Published online by Cambridge University Press:  28 July 2017

Jonathan Labadie-Bartz Open the ORCID record for Jonathan Labadie-Bartz [Opens in a new window] ,
Joshua Pepper ,
S. Drew Chojnowski  and
M. Virginia McSwain
Jonathan Labadie-Bartz
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA; email: jml612@lehigh.edu
Joshua Pepper
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA; email: jml612@lehigh.edu
S. Drew Chojnowski
Affiliation:
Apache Point Observatory and New Mexico State University, P.O. Box 59, Sunspot, NM 88349-0059, USA
M. Virginia McSwain
Affiliation:
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA; email: jml612@lehigh.edu
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Abstract

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We are using light curves from the KELT exoplanet transit survey (Pepper et al. 2007) to study the variability of hundreds of Be stars. Combining these light curves with simultaneous time-series spectra from the APOGEE survey (Majewski et al. 2015) provides a glimpse into how changes in the circumstellar environment are correlated to brightness variations.

Keywords

stars: emission-lineBestars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 418
Copyright
Copyright © International Astronomical Union 2017 

References

Labadie-Bartz, et al., 2017, AJ, 153, 252 CrossRefGoogle Scholar
Majewski, , et al. 2015, arXiv, 1509.05420Google Scholar
Pepper, et al., 2007, PASP, 119, 923 CrossRefGoogle Scholar