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Short-Term Spectroscopic Variations of the Be Star 11 Cam

Published online by Cambridge University Press:  23 September 2016

J. Chauville ,
M. Alvarez ,
J.P. Sareyan ,
L. Ballereau  and
R. Michel
J. Chauville
Affiliation:
UA 337, Observatoire de Meudon, 92190 Meudon, France
M. Alvarez
Affiliation:
UNAM, Instituto de Astronomia, AP 877, Ensenada, Baja Cal. 22860, Mexico
J.P. Sareyan
Affiliation:
Observatoire de Nice, BP 139, 06003 Nice Cedex
L. Ballereau
Affiliation:
UA 337, Observatoire de Meudon, 92190 Meudon, France
R. Michel
Affiliation:
UNAM, Instituto de Astronomia, AP 877, Ensenada, Baja Cal. 22860, Mexico

Extract

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11 Cam (HD 32343 = HR 1622) is a so-called “pole-on” Be star known for its long term variations, already noted by Merrill and Burwell (1943). Recent determinations of visual magnitude and spectral type are V = 5.222 and B2.5Ve (Rufener, 1981). The Balmer line profiles, especially Hα, have been frequently studied; Briot (1971), for instance, measured 40 and 4.9 Å equivalent widths for Hα and Hβ respectively; the Hα/Hβ peak to continuum ratio is 6.43/2.02 according to Gray and Marlborough (1974) who give v sin i = 131 km s-1, close to the value of 140 km s-1 adopted by Kogure (1968).

Type
IIA. The Underlying Stars: Observations
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 93 - 94
Copyright
Copyright © Cambridge University Press 1987

References

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