Semi-empirical Model of the Star V923 Aquilae
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Published:2000
Issue:
Volume:175
Page:547-549
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ISSN:0252-9211
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Container-title:International Astronomical Union Colloquium
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language:en
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Short-container-title:International Astronomical Union Colloquium
Author:
Arias M. L.,Cidale L. S.,Ringuelet A. E.
Abstract
V923 Aquilae (HD 183656) is a Be star which shows emission in Hα, cyclic V/R variations and variations in the near infrared region. This star displays a shell spectrum recognized by Harper(1937) and Bidelman (1950) who both remarked the presence of shell H lines, strong Fe II lines and variable radial velocity. Koubský et al. (1989) proposed V923 Aquilae to be a spectroscopy binary with an orbital period of 214.756 days and a semi-amplitude of 6.2 km/s. Iliev et al. (1994) found a correlation between the changes of the Balmer progression and the asymmetries of the Balmer lines with the orbital phase, considering the period calculated by Koubský.
Publisher
Cambridge University Press (CUP)