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Discrete Structures in the CS Envelope of the Be star ζ Tau

Published online by Cambridge University Press:  12 April 2016

D. Ballereau ,
J. Chauville ,
H. Cao ,
M. Floquet ,
A.M. Hubert  and
J. Zorec
D. Ballereau
Affiliation:
Dasgal, UMR8633 du CNRS, Observatoire de Paris-Meudon, F-92195 Meudon, France
J. Chauville
Affiliation:
Dasgal, UMR8633 du CNRS, Observatoire de Paris-Meudon, F-92195 Meudon, France
H. Cao
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, China
M. Floquet
Affiliation:
Dasgal, UMR8633 du CNRS, Observatoire de Paris-Meudon, F-92195 Meudon, France
A.M. Hubert
Affiliation:
Dasgal, UMR8633 du CNRS, Observatoire de Paris-Meudon, F-92195 Meudon, France
J. Zorec
Affiliation:
Institut d’Astrophysique de Paris - CNRS, 98bis Bd Arago, 75014-Paris, France

Abstract

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The recent cycle of the V/R ratio and RV variations in ζ Tau has been found similar to that reported by Delplace (1970). As a rule, in both cycles, singly-ionized metallic shell lines display discrete components when the descending branch of RV curve of Balmer lines crosses the stellar RV value; a narrow sharp feature is mainly superimposed on a broad and bluer one, both being slowly varying over some months; very weak additional components are suspected on stronger Fe II lines. On another hand, in the ascending branch of RV curve (RV ≥ RVstar), secondary shell components varying in intensity are conspicuous on V and R emissions of the first Balmer lines.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 539 - 542
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

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