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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.)

Cyclic variability of the circumstellar disk of the Be star zeta Tauri II. Testing the 2D global disk oscillation model

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Autor(es):
Carciofi, A. C. [1] ; Okazaki, A. T. [2] ; le Bouquin, J. -B. [3] ; Stefl, S. [3] ; Rivinius, Th. [3] ; Baade, D. [4] ; Bjorkman, J. E. [5] ; Hummel, C. A. [4]
Número total de Autores: 8
Afiliação do(s) autor(es):
[1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508900 Sao Paulo - Brazil
[2] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605 - Japan
[3] ESO European Org Astron Res So Hemisphere, Santiago 19 - Chile
[4] ESO European Org Astron Res So Hemisphere, D-85748 Garching - Germany
[5] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 - USA
Número total de Afiliações: 5
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 504, n. 3, p. 915-927, SEP 2009.
Citações Web of Science: 98
Resumo

Context. About 2/3 of the Be stars present the so-called V/R variations, a phenomenon characterized by the quasi-cyclic variation in the ratio between the violet and red emission peaks of the HI emission lines. These variations are generally explained by global oscillations in the circumstellar disk forming a one-armed spiral density pattern that precesses around the star with a period of a few years. Aims. This paper presents self-consistent models of polarimetric, photometric, spectrophotometric, and interferometric observations of the classical Be star zeta Tauri. The primary goal is to conduct a critical quantitative test of the global oscillation scenario. Methods. Detailed three-dimensional, NLTE radiative transfer calculations were carried out using the radiative transfer code HDUST. The most up-to-date research on Be stars was used as input for the code in order to include a physically realistic description for the central star and the circumstellar disk. The model adopts a rotationally deformed, gravity darkened central star, surrounded by a disk whose unperturbed state is given by a steady-state viscous decretion disk model. It is further assumed that this disk is in vertical hydrostatic equilibrium. Results. By adopting a viscous decretion disk model for zeta Tauri and a rigorous solution of the radiative transfer, a very good fit of the time-average properties of the disk was obtained. This provides strong theoretical evidence that the viscous decretion disk model is the mechanism responsible for disk formation. The global oscillation model successfully fitted spatially resolved VLTI/AMBER observations and the temporal V/R variations in the H alpha and Br gamma lines. This result convincingly demonstrates that the oscillation pattern in the disk is a one-armed spiral. Possible model shortcomings, as well as suggestions for future improvements, are also discussed. (AU)

Processo FAPESP: 04/07707-3 - Envoltórios circunstelares assimétricos
Beneficiário:Alex Cavaliéri Carciofi
Linha de fomento: Bolsas no Brasil - Pós-Doutorado
Processo FAPESP: 04/08851-0 - Facilidades computacionais para o Departamento de Astronomia do IAG-USP
Beneficiário:Ronaldo Eustaquio de Souza
Linha de fomento: Auxílio à Pesquisa - Programa Equipamentos Multiusuários