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A Photometric Study of the Contact Binaries: XY Leo, EE Cet and AQ Psc

Published online by Cambridge University Press:  05 March 2013

Gojko Djurašević
Affiliation:
Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia
Dinko Dimitrov
Affiliation:
Institute of Astronomy, Bulgarian Academy of Sciences, Tzarigradsko Chosse 72, 1784 Sofia, Bulgaria
Bojan Arbutina
Affiliation:
Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia
Berahitdin Albayrak*
Affiliation:
Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, 06100, Tandoğan, Ankara, Turkey
Selim Osman Selam
Affiliation:
Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, 06100, Tandoğan, Ankara, Turkey
Olga Atanacković-Vukmanović
Affiliation:
Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
*
ECorresponding author. E-mail: albayrak@astro1.science.ankara.edu.tr
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Abstract

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New photoelectric BV light curves of three close eclipsing binaries XY Leo, EE Cet and AQ Psc were observed and studied with the aim to derive the physical parameters of these systems. The following results were obtained: (a) the W-type contact binary system XY Leo is in a marginal overcontact configuration (fover ∼ 2.4%) with a relatively large temperature difference between the components (∼330K); (b) due to the proximity of the companion of EE Cet in the visual binary ADS 2163, the light curves of EE Cet were contaminated by the third light, having a relatively large impact on the system-parameter estimates, and the solutions made with the third light parameter, L3 ∼ 0.54, describe EE Cet as a high-overcontact (fover ∼ 33%) W-type system; (c) the A-type W UMa contact eclipsing binary AQ Psc is in an overcontact configuration (fover ∼ 20%). The relatively small temperature difference (∼150K) and large difference in component masses suggest a significant energy transfer through the connecting neck of the common envelope. The absolute system parameters are obtained by combining our photometric solution with the spectroscopic elements given by other authors.

Type
Research Article
Copyright
Copyright © Astronomical Society of Australia 2006

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