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Line Profile Variability in the Be Star α Eridani

Published online by Cambridge University Press:  12 April 2016

N. V. Leister ,
E. Janot-Pacheco ,
J. Leyton Z. ,
A. M. Hubert  and
M. Floquet
N. V. Leister
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, Brazil, 04301-974
E. Janot-Pacheco
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, Brazil, 04301-974
J. Leyton Z.
Affiliation:
Departamento de Física, Universid de la Serena, Chile
A. M. Hubert
Affiliation:
Observatoire de Paris, Section d’Astrophysique de Meudon, UMR 8633 CNRS/DASGAL, F-92195 Meudon Cedex, France
M. Floquet
Affiliation:
Observatoire de Paris, Section d’Astrophysique de Meudon, UMR 8633 CNRS/DASGAL, F-92195 Meudon Cedex, France

Abstract

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We present an analysis of line profile variability of the Be star α Eri (Achernar). Spectra of He I λ667.8nm were collected at Brazilian Laboratório Nacional de Astrofísica (LNA) during 10 observing runs covering 27 nights in 6 years. The presence of a 1.26 days period reported previously is confirmed and we report also the detection of other periods (0.73 and 0.53 days) and a possible 12.5 days modulation. A transient high-velocity absorption component with RV = −500 km/s, higher than −υsini (−220 km/s) has appeared at the end of 1993, near the presumed maximum of the Hα emission phase.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 272 - 275
Copyright
Copyright © Astronomical Society of the Pacific 2000

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