Photometric observations and Numerical modeling of SDSS J162520.29+120308.7, an SU UMa in the CV period gap |
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| Institution: | 1. Department of Physics, University of Central Florida, Orlando, FL 32816, United States;2. Sternberg Astronomical Institute, Moscow State University, Universitetskij prospect 13, Moscow 119992, Russian Federation;3. University of Dallas, 1845 E Northgate Drive, Irving, TX 75062, United States;1. Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551, Japan;2. Earth-Life Science Institute,Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8550, Japan;3. Department of Planetology, Graduate School of Science, Faculty of Science, Kobe University 1-1, Rokkodai-cho, Nada-ku, Kobe, Hyogo, 657-8501, Japan;4. RIKEN Advanced Institute for Computational Science, Minatojima-minamimachi, Chuo-ku, Kobe, Hyogo, 650-0047, Japan;1. Astronomy Dept., National Research Institute of Astronomy and Geophysics, Box: 138, 11421, Helwan, Cairo, Egypt;2. Kottamia Center of Scientific Excellence in Astronomy and Space Sciences (KCScE) STDF, ASRT, Cairo, Egypt;3. Physics Dept., College of Science, Northern Border University, 1320, Arar, Saudi Arabia;4. Astronomy Dept. and Meteorology, Faculty of Science, Al-Azhar University, Cairo, Egypt;1. Via Molinetto 35, 26845 Triulza di Codogno (LO), Italy;2. Via Don G. Minzoni 26/D, 20020 Magnago (MI), Italy;3. Via Zoncada 51, 26845 Codogno (LO), Italy;1. Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV), Berlin, Germany;2. American Association of Variable Star Observers (AAVSO), Cambridge, USA;3. Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic;1. Department of Physics, H.R. Institute of Technology, Ghaziabad - 201003, India;2. Uttrakhand Space Application Centre, Dehradun-248006, India;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 |
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| Abstract: | We present R-band photometric observations of Cataclysmic Variable dwarf nova SU UMa SDSS J162520.29+120308.7 during the July 2010 superoutburst, from near maximum through decline and into a single rebrightening. We find a maximum superoutburst amplitude of ∼ 6.1 magnitudes and a maximum rebrightening amplitude of ∼4 magnitudes. Near superoutburst maximum, we find 0.09604(3) days for the mean Stage B positive superhump period and a much longer period for the hump shaped modulation during the rebrightening. For the orbital period, we find Porb = 0.09113(30) days. As all periods both agree and disagree with values reported by others, additional observations are needed. Our 2015 observations of this system in quiescence reveal a 0.09080(20) day orbital period. As our 2010 value is within the error bars of a spectroscopically determined value and our 2015 photometrically determined value, we suggest 0.09113(30) days as the orbital period for this system. As for the secondary-to-primary mass ratio, analytical models using observed orbital and Stage B positive superhump periods as input suggest q = 0.221. As a check, we present a 3D SPH simulation of the rise to, and during the plateau stage of, the SU UMa in superoutburst, assuming Porb=0.09113 days. For Stages A and B, we find 0.09717 days and 0.09702 days, respectively, for the average simulated positive superhump periods. Analytical models using these simulated Stages A and B and the simulated orbital period suggest q = 0.1920(4) and q = 0.221, respectively, for this system. Due to the poorly constrained observational data and the similar mass ratio estimates regardless of stage, we can neither confirm nor deny that Stage A is better than Stage B for determining mass ratio in CV dwarf novae SU UMa systems. Additional observations and simulations are needed to further test this recently proposed hypothesis. For now, we suggest an average q = 0.21(1) for this system. |
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