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Short-term variations in Be stars observed by the CoRoT and Kepler space missions

Published online by Cambridge University Press:  12 July 2011

Juan Gutiérrez-Soto ,
Coralie Neiner ,
Juan Fabregat ,
Antonino Francesco Lanza ,
Thierry Semaan ,
Monica Rainer  and
Ennio Poretti
Juan Gutiérrez-Soto
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n 18008, Granada, Spain; email: [email protected] LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
Coralie Neiner
Affiliation:
LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
Juan Fabregat
Affiliation:
Observatorio Astronómico de la Universidad de Valencia, Calle Catedrático Agustín Escardino 7, 46980 Paterna, Valencia, Spain
Antonino Francesco Lanza
Affiliation:
INAF - Osservatorio Astrofisico di Catania, via S. Sofia, 78, 95123Catania, Italy
Thierry Semaan
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
Monica Rainer
Affiliation:
INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy
Ennio Poretti
Affiliation:
INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy
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Abstract

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The corot and kepler space missions are collecting very high-precision long-duration photometric data of many Be stars, allowing us to better understand the origin of their short-term variability and the link between these variations and the Be phenomenon. In this paper, we present a brief summary of the results obtained in the analysis of several Be stars observed with corot in terms of pulsations. In addition, we show that variations of the Be star HD 175869 can be explained as two active regions separated by 150 degrees or as unstable pulsating modes in a star with an extensive mixing in radiative layers corresponding to a core overshooting of 0.35Hp. A preliminary study of the photometric and spectroscopic variability seen in the B1.5IVe star HD 51193 is performed. Currently the kepler satellite is observing the only confirmed Be star in its field of view, namely KIC 6954726. From low-resolution spectra we derived a spectral type of B2.5Ve for this star and we studied the long-term variation of the emission in the Hα line. The 3.5-year kepler light curve will allow us to detect even more close frequencies than with corot and to perform a detailed analysis of the amplitude variations in a Be star.

Keywords

stars: oscillationsstars: emission-lineBe
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. 451 - 456
Copyright
Copyright © International Astronomical Union 2011

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