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Photometric study of the eclipsing binary WX Cephei
The photometric elements of the eclipsing binary WX Cep are determinedfrom 3120 photoelectrically measured observations in each of the B and Vregions which were obtained in the summer of 1973 at the Pine MountainObservatory of the University of Oregon. The analysis shows that primaryminimum is produced by the occultation of the smaller, fainter type A2star by the larger brighter star of about type A5, and that during the10.9-hour duration of the primary eclipse it is total for about 40minutes. The existing spectroscopic data (of uncertain quality) for thisdouble-line binary are used to estimate the mass and radius of eachcomponent. Both components have about one solar mass which is somewhatsmaller than expected for these spectral classes even if the luminosityclass of each star is V.
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Observation and Astrometry data
| Constellation: | Κηφεύς |
| Right ascension: | 22h39m57.88s |
| Declination: | +63°34'47.1" |
| Apparent magnitude: | 8.529 |
| Distance: | 213.22 parsecs |
| Proper motion RA: | 11.1 |
| Proper motion Dec: | 5.7 |
| B-T magnitude: | 8.69 |
| V-T magnitude: | 8.543 |
Catalogs and designations:
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