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Non-radial pulsations in the CoRoT Be Star 102761769

Published online by Cambridge University Press:  12 July 2011

Eduardo Janot Pacheco ,
Laerte B.P. de Andrade ,
Marcelo Emilio ,
Juan Carlos Suárez  and
Andressa Jendreieck
Eduardo Janot Pacheco
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil
Laerte B.P. de Andrade
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil
Marcelo Emilio
Affiliation:
Observatorio Astronomico/DEGEO, Universidade Estadual de Ponta Grossa, Av. Carlos Cavalcanti, 4748 Ponta Grossa, / PR, Brazil - 84030-900
Juan Carlos Suárez
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18008 Granada, Spain
Andressa Jendreieck
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil
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Abstract

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We investigate non-radial pulsations of the CoRoT IR1 Be Star 102761769, with a projected stellar rotation estimated to be 120±15 km/s. If the star is a typical galactic Be star it rotates near the critical velocity. We propose an alternative scenario, where the star could be seen nearly equator-on rotating at a relatively moderate velocity say, ≈ 120 km/s and therefore the nonradial oscillations could be modeled. In order to identify the pulsation modes of the observed frequencies, we computed a set of models representative of CoRoT 102761769 by means of the adiabatic pulsation package FILOU. Results indicate that the two frequencies are compatible with a high-g mode as predicted by pulsation models of Be stars.

Keywords

stars: oscillations (including pulsations)stars: rotationstars: 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. 507 - 508
Copyright
Copyright © International Astronomical Union 2011

References

Emilio, M., Andrade, L., Janot-Pacheco, E., & Baglin, A. et al. 2010, A&A, 522A, 43Google Scholar
Huang, W. & Gies, D. R. 2006, ApJ, 648, 591CrossRefGoogle Scholar
Morel, P. 1997, A&AS, 124, 597Google Scholar
Suárez, J. C., Goupil, M. J., & Morel, P. 2006, A&A, 449, 673Google Scholar
Suárez, J. C. & Goupil, M. J. 2008, Ap&SS, 316, 155Google Scholar
Suárez, J. C., Moya, A., Amado, P. J., & Martín-Ruiz, S. et al. 2009, ApJ, 690, 1401CrossRefGoogle Scholar
Tran Minh, F., & Léon, L. 1995, in: Roxburgh, I. W. & Masnou, J.-L. (eds.) Physical Processes in Astrophysics, p. 219Google Scholar