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Eta Orionis

Published online by Cambridge University Press:  12 April 2016

K. De Mey ,
C. Aerts ,
H. Van Winckel  and
C. Waelkens
K. De Mey
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
C. Aerts
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
H. Van Winckel
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
C. Waelkens
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium

Extract

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Eta Orionis is an interesting multiple system of early type stars. It consists of a visual triple system (A, B, C), a spectroscopic triple system (Aabc) and an eclipsing binary Aab. A is a triple system consisting of a 7.989 day eclipsing binary Aab and a gravitationally bound third component Ac with orbital period of about 9.5 years. All components of the pair AB have spectral types in the range 09-B3 (C. Waelkens & P. Lampens 1988). The radial velocity curve is used to constrain the orbital elements and properties of the binary Aab.

The second component Ab is a B-type star that displays rapid absorption line profile variability. Regular patterns are easily visible in the data.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 311 - 312
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

Aerts, C., De Pauw, M., & Waelkens, C. 1992, A&A, 266, 294 Google Scholar
Waelkens, C., & Lampens, P. 1988, A&A, 194, 143 Google Scholar