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The orbital period study and photometric analysis of XY Ursae Majoris
Photoelectric observations of the eclipsing binary XY UMa have beencarried out in B and V colours at the Ege University Observatory.Combining these newly obtained data with the previous ones available inthe literature, the problem pertaining to the orbital period of thesystem has been investigated through a detailed description of the O-Cdiagram. The sinusoidal and secular changes have been found. Suchvariations of the orbital period have been examined in terms of threeplausible mechanisms, namely (i) a light-time effect due to a thirdbody, (ii) the orbital period modulation due to magnetic activity cycleof a component star, and (iii) a mass loss case in which the ejectedmaterial escapes out from the binary system. A combination of a magneticactivity cycle mechanism and a mass loss case is found to reproducesatisfactorily the period changes. Further, the observed photoelectriclight curves of the system have been analyzed with the Wilson-Devinneyapproach. This analysis shows that the asymmetries of the light curvesof XY UMa can be interpreted in terms of cool star-spot covering 7% ofthe stellar photosphere of the primary component of this binary. Thesystem is found to be a beta Lyrae type detached binary. The absoluteelements of the system are also deduced.
| Photoelectric Light Curves and Minimum Times of XY UMa
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Osservazione e dati astrometrici
| Costellazione: | Orsa Maggiore |
| Ascensione retta: | 09h06m20.30s |
| Declinazione: | +54°00'11.9" |
| Magnitudine apparente: | 9.37 |
| Moto proprio RA: | -16 |
| Moto proprio Dec: | -10.8 |
| B-T magnitude: | 10.966 |
| V-T magnitude: | 9.502 |
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