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Semi-empirical Model of the Star V923 Aquilae

Published online by Cambridge University Press:  12 April 2016

M. L. Arias ,
L. S. Cidale  and
A. E. Ringuelet
M. L. Arias
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900, La Plata, Argentina
L. S. Cidale
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900, La Plata, Argentina
A. E. Ringuelet
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900, La Plata, Argentina

Extract

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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.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 547 - 549
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Bidelman, W.P. 1950, PASP 62, 48.Google Scholar
Cidale, L., Ringuelet, A.E. 1989, PASP 101, 417.Google Scholar
Harper, W.E. 1937, Pub. Dominion Astrophys. Obs. 7, 1.Google Scholar
Iliev, L. 1994, “Pulsation, rotation and mass loss in early type stars”, IAU Symp. 162, p.374.Google Scholar
Jefferies, J.T., “Spectral Line Formation”, Ed. Blaisdell Publishing and Company, 1968.Google Scholar
Koubský, et al. 1989, Space Sci.Rev. 50, 377.Google Scholar
Koubský, et al. 1989, Bull. Astron. Inst. Czechosl. 40, 31–41.Google Scholar