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Call H and K Emission in the Secondary Component of U Cephei

Published online by Cambridge University Press:  12 April 2016

Akira Okazaki ,
Yasuhisa Nakamura  and
Jun-Ichi Katahira
Akira Okazaki
Affiliation:
Tsuda College, Kodaira, Tokyo 187, Japan
Yasuhisa Nakamura
Affiliation:
Komaba Senior High School, Meguro-ku, Tokyo 153, Japan
Jun-Ichi Katahira
Affiliation:
Science EducationInstitute of Sakai, Sakai 591, Japan

Extract

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U Cephei (V = 6.8–9.0, P = 2.493 d) is an eclipsing binary consisting of a B7V primary and a G8III-IV secondary component. This binary is one of the semidetached Algol systems showing soft X-ray emission which is probably associated with a hot corona surrounding the secondary component (White and Marshall 1983).

We made spectroscopic observations of U Cep with the coudé image-tube spectrograph of the 1.9-m telescope at Okayama Astrophysical Observatory on October 14, 1986. We obtained four spectrograms with a dispersion of 16 Å mm-1 covering λ λ3700—4300 Å during the primary eclipse. The first two exposures were made in a total eclipse, while the last two were slightly after the third contact. The CaII H and K emission lines appear clearly in all the spectrograms. Figure 1 represents an intensity tracing of one of these spectrograms.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 219 - 220
Copyright
Copyright © Springer-Verlag 1988

References

Linsky, J.L., Worden, S.P., McClintock, W., and Robertson, R.M.: 1979, Astrophys. J. Suppl., 41, 47 Google Scholar
White, N.E., and Marshall, F.E.: 1983, Astrophys. J. Letter, 268, L117.CrossRefGoogle Scholar