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Phase Variation and NRP Modes in Southern Be Stars

Published online by Cambridge University Press:  12 April 2016

E. Janot-Pacheco ,
N.V. Leister ,
A.D. de Souza Jr ,
S. Jankov ,
A.M. Hubert  and
M. Floquet
E. Janot-Pacheco
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, 04301-974 São Paulo, Brazil
N.V. Leister
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, 04301-974 São Paulo, Brazil
A.D. de Souza Jr
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, 04301-974 São Paulo, Brazil
S. Jankov
Affiliation:
Astronomska Opservatorija Beograd, Volgina 7, 11050 Beograd, Yuguslaviag
A.M. Hubert
Affiliation:
Dasgal, UMR8633, Observatoire de Meudon, 92195 Meudon Cedex, France
M. Floquet
Affiliation:
Dasgal, UMR8633, Observatoire de Meudon, 92195 Meudon Cedex, France

Abstract

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ζ Ophiuchi and η Centauri are hot, rapidly rotating, southern Be stars showing multi-mode nonradial pulsations (nrp). We use high resolution, high signal-to-noise ratio spectroscopic observations of these objects to test the Telting and Schrijvers’ method (TS) of mode degree l and azimuthal order | m | estimation. In this method, these quantum numbers are calculated from the blue-to-red phase difference of the corresponding main frequency and its first harmonic, respectively. The phase differences were obtained withe the help of the Clean and Cleanest algorithms. Quantum numbers calculated with TS are compatible with those obtained with the Fourier Doppler method within the estimated errors. In the absence of other tools, the TS method can thus be used to estimate l and | m | with reasonably accuracy.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 248 - 251
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Foster, G. 1995, AJ 109, 1889 CrossRefGoogle Scholar
Jankov, S., Janot-Pacheco, E., Leister, N.V. 1999, ApJ, in the pressGoogle Scholar
Janot-Pacheco, E. et al. 1999, A&AS 137, 407 Google Scholar
Kambe, E., Ando, H., Hirata, R. 1990, PASJ 42, 687 Google Scholar
Kennelly, E.J. et al. 1992, ApJ 400, L71 CrossRefGoogle Scholar
Roberts, D.H., Lehar, J., Dreher, J.W. 1987, AJ 93, 968 Google Scholar
Schrijvers, C. et al. 1997, A&AS 121, 343 Google Scholar
Souza, A. Jr., et al. 1999, this meetingGoogle Scholar
Telting, J.H., Schrijvers, C. 1997a, A&A 317, 723 Google Scholar
Telting, J.H., Schrijvers, C. 1997b, A&A 327, 579 Google Scholar