Huat, A.-L. ; Hubert, A.-M. ; Baudin, F. ; Floquet, M. ; Neiner, C. ; Frémat, Y. ; Gutiérrez-Soto, J. ; Andrade, L. ; de Batz, B. ; Diago, P. D. ; Emilio, M. ; Espinosa Lara, F. ; Fabregat, J. ; Janot-Pacheco, E. ; Leroy, B. ; Martayan, C. ; Semaan, T. ; Suso, J. ; Auvergne, M. ; Catala, C. ; Michel, E. ; Samadi, R.

published in Astronomy and Astrophysics, 506, pp. 95-101 (2009)

Abstract: Context: Be stars undergo outbursts producing a circumstellar disk from the ejected material. The beating of non-radial pulsations has been put forward as a possible mechanism of ejection. Aims: We analyze the pulsational behavior of the early B0.5IVe star HD 49330 observed during the first CoRoT long run towards the Galactical anticenter (LRA1). This Be star is located close to the lower edge of the ß Cephei instability strip in the HR diagram and showed a 0.03 mag outburst during the CoRoT observations. It is thus an ideal case for testing the aforementioned hypothesis. Methods: We analyze the CoRoT light curve of HD 49330 using Fourier methods and non-linear least square fitting. Results: In this star, we find pulsation modes typical of ß Cep stars (p modes) and SPB stars (g modes) with amplitude variations along the run directly correlated with the outburst. These results provide new clues about the origin of the Be phenomenon as well as strong constraints on the seismic modelling of Be stars. Tables 3 to 7 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/95

DOI: 10.1051/0004-6361/200911928
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