Pulsations in the late-type Be star HD 50 209 detected by CoRoT

被引：30

作者：

Diago, P. D. ^{[1
]}

Gutierrez-Soto, J. ^{[2
,3
]}

Auvergne, M. ^{[3
]}

Fabregat, J. ^{[1
]}

Hubert, A. -M. ^{[2
]}

Floquet, M. ^{[2
]}

Fremat, Y. ^{[2
,4
]}

Garrido, R. ^{[5
]}

Andrade, L. ^{[6
]}

de Batz, B. ^{[2
]}

Emilio, M. ^{[7
]}

Lara, F. Espinosa ^{[2
]}

Huat, A. -L. ^{[2
]}

Janot-Pacheco, E. ^{[6
]}

Leroy, B. ^{[3
]}

Martayan, C. ^{[2
,4
]}

Neiner, C. ^{[2
]}

Semaan, T. ^{[2
]}

Suso, J. ^{[1
]}

Catala, C. ^{[3
]}

Poretti, E. ^{[8
]}

Rainer, M. ^{[8
]}

Uytterhoeven, K. ^{[8
,9
]}

Michel, E. ^{[3
]}

Samadi, R. ^{[3
]}

机构：

[1] Univ Valencia, Astron Observ, Valencia 46980, Spain

[2] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92195 Meudon, France

[3] Univ Paris Diderot, CNRS, Observ Paris, LESIA, F-92195 Meudon, France

[4] Royal Observ Belgium, B-1180 Brussels, Belgium

[5] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain

[6] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer IAG, Dept Astron, BR-05508900 Sao Paulo, Brazil

[7] Univ Estadual Ponta Grossa, Observ Astron DEGEO, BR-4748 Ponta Grossa, Parana, Brazil

[8] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy

[9] Inst Astrofis Canarias, San Cristobal la Laguna 38205, TF, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2009年 / 506卷 / 01期

关键词：

stars: emission line; Be; stars: oscillations; stars: individual: HD 50 209; FUNDAMENTAL PARAMETERS; SEISMOLOGY FIELDS; SPACED DATA; G-MODES; VARIABILITY;

D O I：

10.1051/0004-6361/200911901

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The presence of pulsations in late-type Be stars is still a matter of controversy. It constitutes an important issue to establish the relationship between non-radial pulsations and the mass-loss mechanism in Be stars. Aims. To contribute to this discussion, we analyse the photometric time series of the B8IVe star HD 50 209 observed by the CoRoT mission in the seismology field. Methods. We use standard Fourier techniques and linear and non-linear least squares fitting methods to analyse the CoRoT light curve. In addition, we applied detailed modelling of high-resolution spectra to obtain the fundamental physical parameters of the star. Results. We have found four frequencies which correspond to gravity modes with azimuthal order m = 0,-1,-2,-3 with the same pulsational frequency in the co-rotating frame. We also found a rotational period with a frequency of 0.679 cd(-1) (7.754 mu Hz). Conclusions. HD 50 209 is a pulsating Be star as expected from its position in the HR diagram, close to the SPB instability strip.

引用

页码：125 / 131

页数：7

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