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Ultraviolet Observations of CX Draconis

Published online by Cambridge University Press:  23 September 2016

P. Koubský ,
J. Horn ,
P. Harmanec ,
G. J. Peters ,
R. S. Polidan  and
P. K. Barker
P. Koubský
Affiliation:
Astron. Institute, 25165 Ondrejov, Czechoslovakia
J. Horn
Affiliation:
Astron. Institute, 25165 Ondrejov, Czechoslovakia
P. Harmanec
Affiliation:
Astron. Institute, 25165 Ondrejov, Czechoslovakia
G. J. Peters
Affiliation:
Dept. of Astronomy, USC, Los Angeles, 90080, U.S.A
R. S. Polidan
Affiliation:
LPL, University of Arizona, Tucson, 85713, U.S.A.
P. K. Barker
Affiliation:
Astron. Department, UWO, London, N, 6A5B9, Canada

Extract

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CX Draconis /HD 174237, B2.5Ve, v.sin i = 160 km.s-1/ is a typical Be star displaying most of the well known spectroscopic and photometric characteristics of these stars.

Koubský /1978/ disclosed that CX Dra is a SB1 /P=6.69603d, K = 35 km.s-1, e = 0/. Penrod /1985/ confirmed that the secondary is a F star. Peters and Polidan /1984/ reported strong, variable lines of NV, CIV and SilV from high-resolution spectra secured with IUE satellite. These features were interpreted to arise from gas stream and accretion close to the photosphere of the B-component of the system.

Type
IV. Models
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 443 - 444
Copyright
Copyright © Cambridge University Press 1987

References

Koubsky, P. /1978/. BAC 29, 288 Google Scholar
Penrod, G.D., /1985/. Private communicationGoogle Scholar
Peters, G.J., and Polidan, R.S. /1984/. ApJ 233, 745 Google Scholar