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A Pulsational Study of a Sample of CoRoT Faint Be Stars

  • T. SemaanEmail author
  • J. Gutiérrez-Soto
  • Y. Frémat
  • A. M. Hubert
  • C. Martayan
  • J. Zorec
Chapter
Part of the Astrophysics and Space Science Proceedings book series (ASSSP, volume 31)

Abstract

We present an intensive study of a sample of 12 Be stars in the first exo-planetary fields of the CoRoT mission. The aim is to understand the short-term variability in Be stars. We use both spectroscopic and photometric data: VLT-GIRAFFE spectra to derive the fundamental parameters and CoRoT light curves to search for low-amplitude frequencies. This allows us to locate the stars in the HR diagram and compare their positions in the instability strip with those of other pulsating B stars. From VLT-GIRAFFE observations we determined the stellar parameters by fitting the observed spectra with non-LTE stellar atmosphere models. The observed spectra were corrected for veiling effects due to circumstellar material and for rotational effects. We estimated the rotational frequency using the corrected fundamental parameters. For the CoRoT light curves, we determined all significant frequencies and compared the main frequencies with the rotational frequency. We also investigated the variation of the frequencies and amplitudes with time and, in particular, during outbursts. This is the first time that a statistical study with space data has been performed for Be stars. Our study suggests that rotational modulation is not the cause of short-term photometric variability in Be stars.

Notes

Acknowledgements

This research is based on CoRoT data. The CoRoT (Convection, Rotation and planetary Transits) space mission, launched on December 27th 2006, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA, Germany and Spain.

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Copyright information

© Springer-Verlag Berlin Heidelberg 2013

Authors and Affiliations

  • T. Semaan
    • 1
    Email author
  • J. Gutiérrez-Soto
    • 2
  • Y. Frémat
    • 3
  • A. M. Hubert
    • 1
  • C. Martayan
    • 4
  • J. Zorec
    • 5
  1. 1.GEPI, Observatoire de ParisParisFrance
  2. 2.Valencian International University & Instituto de Astrofisica de Andalucia (CSIC)ValencianSpain
  3. 3.Royal Observatory of BelgiumUkkelBelgium
  4. 4.ESOSantiagoChile
  5. 5.UPMC, CNRS, UMR 7095, Institut d’Astrophysique de ParisParisFrance

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