Photometric observations and numerical modeling of AW Sge |
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| Institution: | 1. Department of Physics, University of Central Florida, Orlando, FL 32816, USA;2. Sternberg Astronomical Institute, Moscow State University, Universitetskij prospect 13, Moscow 119992, Russia;3. Institute for Simulation and Training, University of Central Florida, Orlando, FL 32816, USA;1. Astrophysics Research Centre and Observatory, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020, Çanakkale, Turkey;2. Department of Physics, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020, Çanakkale, Turkey;3. Department of Space Sciences and Technologies, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020, Çanakkale, Turkey;4. Department of Physics, University of Johannesburg, PO Box 524, Auckland Park 2006, South Africa;5. South African Astronomical Observatory, PO Box 9, Observatory, 7935, South Africa;6. Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa;7. Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, bus 2401, B-3001 Leuven, Belgium;1. Department of Physics, University of Kashmir, Hazratbal, Srinagar, Jammu and Kashmir 190006, India;2. Islamia College of Science and Commerce, Hawal, Srinagar, Jammu and Kashmir 190002, Inida;3. Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India;4. Applied Sciences Department, Gowhati University, Assam, India;1. High Energy Physics Division, Argonne National Laboratory, Lemont, IL 60439, USA;2. Mathematics and Computer Science Division, Argonne National Laboratory, Lemont, IL 60439, USA;3. Kavli Institute for Cosmological Physics, The University of Chicago, 5640 S. Ellis Ave., Chicago, IL 60637, USA;4. Computation Institute, The University of Chicago, Chicago, IL 60637, USA;5. Argonne Leadership Computing Facility, Argonne National Laboratory, Lemont IL 60439, USA;6. Department of Physics, University of Chicago, Chicago, IL 60637, USA;7. Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA;8. Kitware, 28 Corporate Drive, Clifton Park, NY 12065, USA;9. Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 90095, USA;10. Department of Electrical Engineering and Computer Science, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA;1. INAF- Catania Astrophysical Observatory, via S.Sofia 78, Catania, I-95123, Italy;2. Klein Karoo Observatory, Western Cape, South Africa;3. South African Astronomical Observatory, P.O. Box 9, Observatory, 7935, South Africa;4. Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK |
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| Abstract: | In this work, we present R-band photometric light curves of Cataclysmic Variable AW Sge, an SU Uma type, near superoutburst maximum. The positive superhump shape changes over three days, from single peaked on October 11, 2013 to one maximum near phase ? ～ 0.3 followed by minor peaks near phases ? ～ 0.6 and ? ～ 0.9, respectively, on October 13, 2013. Using the maxima from October 11–13, 2013 (JD 2456577–2356579), the observed positive superhump period is 0.074293 ± 0.000025 days.In addition to the observations, we also provide a three dimensional Smoothed Particle Hydrodynamic simulation near superoutburst maximum, for comparison, assuming a secondary-to-primary mass ratio = 0.6 M⊙/0.132 M⊙ = 0.22. The simulation produces positive superhump shapes that are similar to the observations. The simulated positive superhump has a period of 0.076923 days, which is approximately 6% longer than the orbital period, assuming an orbital period Porb = 0.0724 days. The 3.5% difference from the observed positive superhump period is likely due to the assumptions used in generating the simulations, as the orbital period and masses are not well known. From an analysis of the simulated positive superhump shape near superoutburst maximum, the maximum occurs near ? ～ 0.3, when the disk is highly elliptical and eccentric and at least one of the two density waves is compressing with the disk rim. Based on the simulation, we find that the disk may be tilted and precessing in the retrograde direction at a time that is just before the next outburst and/or superoutburst. |
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