Photometric variability of the Be star CoRoT-ID 102761769⋆

Author： Emilio M.   Andrade L.   Janot-Pacheco E.   Baglin A.   Gutiérrez-Soto J.   Suárez J. C.   de Batz B.   Diago P.   Fabregat J.   Floquet M.   Frémat Y.   Huat A. L.   Hubert A. M.   Espinosa Lara F.   Leroy B.   Martayan C.   Neiner C.   Semaan T.   Suso J.  

Publisher： Edp Sciences

E-ISSN： 1432-0746|522|issue|A43-A43

ISSN： 0004-6361

Source： Astronomy & Astrophysics, Vol.522, Iss.issue, 2010-10, pp. : A43-A43

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Abstract

Context. Classical Be stars are rapid rotators of spectral type late O to early A and luminosity class V-III, which exhibit Balmer emission lines and often a near infrared excess originating in an equatorially concentrated circumstellar envelope, both produced by sporadic mass ejection episodes. The causes of the abnormal mass loss (the so-called Be phenomenon) are as yet unknown.

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