New CCD photometry of the eclipsing binary system V1067 Her |
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| Institution: | 1. Astronomy Dept. and Meteorology, Faculty of Science, Al-AzharUniversity, Cairo, Egypt;2. Astronomy Dept., National Research Institute of Astronomy and Geophysics, Helwan, Cairo, Egypt;3. Kottamia Center of Scientific Excellence in Astronomy and Space Sciences (KCScE), Cairo, Egypt;1. Florida Institute of Technology, Physics and Space Sciences Department, Melbourne, Florida, 32901, USA;2. Florida Institute of Technology, Systems Engineering Department, Melbourne, Florida, 32901, USA;1. Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Konkoly Thege Miklós út 15-17, Hungary;2. BSObservatory, Modrá 587, Zlín 760 01, Czech Republic;1. Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV), Berlin, Germany;2. American Association of Variable Star Observers (AAVSO), Cambridge, USA;3. Vereniging Voor Sterrenkunde (VVS), Brugge, Belgium;4. Astrolab IRIS, Ieper, Belgium;5. Department of Physics, University of Warwick, Coventry, United Kingdom;6. Center for Plasma Astrophysics, University of Leuven, Belgium |
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| Abstract: | We present a new set of CCD photometric observations for the short period eclipsing binary 1SWASP J1743 (= V1067 Her). We have determined the available times of light minima and two new linear and quadratic ephemerides have been obtained. The photometric solutions for the system have been performed using Wilson and Devinney Code. The 3D and fill out configuration revealed that V1067 Her is an over contact W UMa binary with relatively low fill-out factor of about 16%.We investigated the period variation for the system. It showed a strong evidence of period changes by using the (O-C) residual diagram method and we have concluded long-term orbital period decrease rate dP/dt= −3.0 × 10−7 d/yr, corresponding to a time scale 8.6 × 105 yr. Such period decrease in the A-type W UMa systems is usually interpreted to be due to mass transfer from the more to the less massive component. |
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