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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Photometric variability of the Be star CoRoT-ID 102761769

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Autor(es):
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Emilio, M. [1] ; Andrade, L. [2] ; Janot-Pacheco, E. [2] ; Baglin, A. [3] ; Gutierrez-Soto, J. [4] ; Suarez, J. C. [5] ; de Batz, B. [6] ; Diago, P. [4, 5] ; Fabregat, J. [4] ; Floquet, M. [6] ; Fremat, Y. [7] ; Huat, A. L. [6] ; Hubert, A. M. [6] ; Lara, F. Espinosa [6] ; Leroy, B. [3] ; Martayan, C. [6, 8] ; Neiner, C. [6] ; Semaan, T. [6] ; Suso, J. [4]
Número total de Autores: 19
Afiliação do(s) autor(es):
[1] Univ Estadual Ponta Grossa, Observ Astron DEGEO, BR-84030900 Ponta Grossa, PR - Brazil
[2] Univ Sao Paulo IAG USP, BR-05508900 Sao Paulo - Brazil
[3] Univ Paris Diderot, CNRS, Observ Paris, Observ Meudon LESIA, F-92190 Meudon - France
[4] Univ Valencia, Astron Observ, Edifici Inst Invest, Valencia 46980 - Spain
[5] Inst Astrofis Andalucia CSIC, Granada - Spain
[6] Univ Paris Diderot, Observ Meudon GEPI, Observ Paris, CNRS, F-92190 Meudon - France
[7] Royal Observ Belgium, B-1180 Brussels - Belgium
[8] European Org Astron Res So Hemisphere, Santiago - Chile
Número total de Afiliações: 8
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 522, NOV 2010.
Citações Web of Science: 7
Resumo

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. Aims. For the first time, we can now study in detail Be stars outside the Earth's atmosphere with sufficient temporal resolution. We investigate the variability of the Be Star CoRoT-ID 102761769 observed with the CoRoT satellite in the exoplanet field during the initial run. Methods. One low-resolution spectrum of the star was obtained with the INT telescope at the Observatorio del Roque de los Muchachos. A time series analysis was performed using both cleanest and singular spectrum analysis algorithms to the CoRoT light curve. To identify the pulsation modes of the observed frequencies, we computed a set of models representative of CoRoT-ID 102761769 by varying its main physical parameters inside the uncertainties discussed. Results. We found two close frequencies related to the star. They are 2.465 c d(-1) (28.5 mu Hz) and 2.441 c d(-1) (28.2 mu Hz). The precision to which those frequencies were found is 0.018 c d(-1) (0.2 mu Hz). The projected stellar rotation was estimated to be 120 km s(-1) from the Fourier transform of spectral lines. If CoRoT-ID 102761769 is a typical Galactic Be star it rotates near the critical velocity. The critical rotation frequency of a typical B5-6 star is about 3.5 c d(-1) (40.5 mu Hz), which implies that the above frequencies are really caused by stellar pulsations rather than star's rotation. (AU)

Processo FAPESP: 05/58746-1 - Centro de Análise Temporal CoRoT
Beneficiário:Eduardo Janot Pacheco
Linha de fomento: Auxílio à Pesquisa - Regular
Processo FAPESP: 06/50341-5 - Centro de análise temporal CoRoT (CAT-CoRoT)
Beneficiário:Eduardo Janot Pacheco
Linha de fomento: Auxílio à Pesquisa - Regular