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Photometric study of the short period W UMa system - FZ Orionis
Photoelectric B, V observations of the eclipsing binary system FZOrionis obtained from the Japal-Rangapur Observatory during the years1981 to 1992 are presented and studied. No period changes in the systemare detected. The light curves are analysed using the Wilson-Devinneymethod and the system parameters are derived.
| FZ Orionis: A short period W UMa system
Photoelectric U, B, and V observations of the eclipsing binary system FZOrionis obtained by the author during three years 1984, 1985 and 1986are presented and studied. The present photometry may settle the disputeregarding the class and the period of the system light variation bewteenthe GCVS 1969 (Beta Lyr; p = 1.597 d) and Figer (1983) and Le Brogne etal (1984) (W UMa; p approximately equals 0.4 d) in favour of the latter.A period change was detected which may be elucidated as due to thepresence of a third body and mass exchange between the components. Timesof ten minima were determined and new ephemeris have been deduced. Thepresent light and color curves were investigated and preliminaryparameters for the system could be estimated.
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Member of following groups:
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Observation and Astrometry data
| Constellation: | Orion |
| Right ascension: | 05h41m21.18s |
| Declination: | +02°21'40.7" |
| Apparent magnitude: | 8.628 |
| Distance: | 269.542 parsecs |
| Proper motion RA: | 0.1 |
| Proper motion Dec: | -16.7 |
| B-T magnitude: | 9.395 |
| V-T magnitude: | 8.692 |
Catalogs and designations:
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INHABITED SKY
