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Multi-frequency Variations in the Be star ζ Ophiuchi

Published online by Cambridge University Press:  12 April 2016

A.D. de Souza Jr ,
E. Janot-Pacheco ,
N.V. Leister ,
S. Jankov ,
A.M. Hubert  and
M. Floquet
A.D. de Souza Jr
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, C.P. 3386, 01060-970, São Paulo, SP, Brasil
E. Janot-Pacheco
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, C.P. 3386, 01060-970, São Paulo, SP, Brasil
N.V. Leister
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, C.P. 3386, 01060-970, São Paulo, SP, Brasil
S. Jankov
Affiliation:
Astronomska Opservatorija Beograd, Volgina 7, 11050 Beograd, Yugoslavia
A.M. Hubert
Affiliation:
Dasgal, UMR 8633 DU CNRS, Observaroire de Meudon, 92195 Meudon, France
M. Floquet
Affiliation:
Dasgal, UMR 8633 DU CNRS, Observaroire de Meudon, 92195 Meudon, France

Abstract

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In this work we have adopted the non radial pulsation (NRP) model in order to explain the rapid spectroscopic time variations observed in the Be star ζ Ophiuchi. Time series analysis were performed with CLEAN and Sequential CLEANEST techniques. We have also applied a different version of the Local CLEANEST that is optimized for multiperiodic signals observed in monosite campaigns. The frequencies of 7.19 and 11.89 cycles/day have been identified. These frequencies were found in previous papers about the star.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 276 - 279
Copyright
Copyright © Astronomical Society of the Pacific 2000

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