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Survey for δ Sct components in eclipsing binaries and new correlations between pulsation frequency and fundamental stellar characteristics

Authors

  • A. Liakos,

    Corresponding author
    1. Department of Astrophysics, Astronomy and Mechanics, University of Athens, GR-157 84 Zografos, Athens, Greece
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  • P. Niarchos,

    1. Department of Astrophysics, Astronomy and Mechanics, University of Athens, GR-157 84 Zografos, Athens, Greece
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  • E. Soydugan,

    1. Department of Physics, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University & Çanakkale Onsekiz Mart University Observatory, Terzioǧlu Campus, TR-17020 Çanakkale, Turkey
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  • P. Zasche

    1. Astronomical Institute, Faculty of Mathematics and Physics, Charles University Prague, CZ-180 00 Praha 8, V Holešovičkách 2, Czech Republic
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E-mail: alliakos@phys.uoa.gr

ABSTRACT

CCD observations of 68 eclipsing binary systems, candidates for containing δ Scuti components, were obtained. Their light curves are analysed using the period04 software for possible pulsational behaviour. For the systems QY Aql, CZ Aqr, TY Cap, WY Cet, UW Cyg, HL Dra, HZ Dra, AU Lac, CL Lyn and IO UMa, complete light curves were observed due to the detection of a pulsating component. All of them, except QY Aql and IO UMa, are analysed with modern astronomical softwares in order to determine their geometrical and pulsational characteristics. Spectroscopic observations of WY Cet and UW Cyg were used to estimate the spectral class of their primary components, while for HZ Dra radial velocities of its primary were measured. O − C diagram analysis was performed for the cases showing peculiar orbital period variations, namely CZ Aqr, TY Cap, WY Cet and UW Cyg, with the aim of obtaining a comprehensive picture of these systems. An updated catalogue of 74 close binaries including a δ Scuti companion is presented. Moreover, a connection between orbital and pulsation periods, as well as a correlation between evolutionary status and dominant pulsation frequency for these systems, is discussed.

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