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      저자 : N. S. AWADALLA (검색결과 2 건)
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      • SCIESCOPUSKCI등재

        ABSOLUTE PARAMETERS AND MASS-RADIUS-LUMINOSITY RELATIONS FOR THE SUB-TYPES OF W UMα BINARIES

        AWADALLA N. S.,HANNA M. A. The Korean Astronomical Society 2005 Journal of The Korean Astronomical Society Vol.38 No.2

        The authors have assembled a sample of 80 W UMa binary systems (42 W-subtype and 38 A-subtype) whose light curves have all been solved by means of the recent W-D code and combined with up-to-date radial velocity solutions. The absolute parameters (masses, radii and luminosities) have been derived (without any constraint on the physical parameters). The main results of this paper are: (1) the mass-luminosity relations for both W&A-subtypes. as well as for all W UMa contact binaries have been shown, (2) the mass-radius relations have been found for both subtypes, (3) some remarks on the evolution status have been presented.

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        NEW CCD OBSERVATIONS AND THE FIRST PHOTOMETRIC STUDY OF THE CONTACT BINARY AP UMI

        N. S. AWADALLA,M. A. HANNA,M. N. Ismail,I. A. Hassan,M. A. Elkhamisy 한국천문학회 2016 Journal of The Korean Astronomical Society Vol.49 No.3

        We obtain the first complete CCD light curves (LCs) of the contact binary AP UMi in the VRI bands and analyzed them by means of the PHOEBE code. A spotted model is applied to treat the asymmetry in the LCs. The LC morphology clearly shows the O'Connell effect and the solution shows an influence of star spots on both components. Such effect of star spots is common between the RS CVn and W UMa chromospherically active stars. Based on the obtained solution of the LCs we investigate the evolutionary state of the components and conclude that the system is a pre-intermediate contact binary ($f=0.29$) with mass ratio $q=0.38$, and it is an A-type W UMa system where the less massive secondary component is cooler than the more massive primary one.} We obtain the first complete CCD light curves (LCs) of the contact binary AP UMi in the VRI bands and analyzed them by means of the PHOEBE code. A spotted model is applied to treat the asymmetry in the LCs. The LC morphology clearly shows the O'Connell effect and the solution shows an influence of star spots on both components. Such effect of star spots is common between the RS CVn and W UMa chromospherically active stars. Based on the obtained solution of the LCs we investigate the evolutionary state of the components and conclude that the system is a pre-intermediate contact binary ($f=0.29$) with mass ratio $q=0.38$, and it is an A-type W UMa system where the less massive secondary component is cooler than the more massive primary one.

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