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Title:
DQ Herculis in Profile: Whole Earth Telescope Observations and Smoothed Particle Hydrodynamics Simulations of an Edge-on Cataclysmic Variable System
Authors:
Wood, M. A.; Robertson, J. R.; Simpson, J. C.; Kawaler, S. D.; O'Brien, M. S.; Nather, R. E.; Winget, D. E.; Montgomery, M. H.; Metcalfe, T. S.; Jiang, X. J.; Leibowitz, E. M.; Ibbetson, P.; O'Donoghue, D.; Zola, S.; Krzesinski, J.; Pajdosz, G.; Vauclair, G.; Dolez, N.; Chevreton, M.; Sullivan, D. J.; Kanaan, A.; Nitta, A.
Affiliation:
AA(Department of Physics and Space Sciences and SARA Observatory, Florida Institute of Technology, Melbourne, FL 32901-6975 .), AB(Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608. Current address: Department of Physics and Space Sciences, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901-6988.; Southeastern Association for Research in Astronomy, NSF-REU Summer Intern.), AC(Range Systems Design and Development Branch, NASA YA-D7, Kennedy Space Center, FL 32899.), AD(Department of Physics, Iowa State University, Ames, IA 50011.), AE(Department of Physics, Iowa State University, Ames, IA 50011.; Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06511.), AF(Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712.), AG(Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712.), AH(Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712.; Institute for Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 OHA, UK.), AI(Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712.; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Mail Stop 16, Cambridge, MA 02138.), AJ(Beijing Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences, 20 Datun Road, Chaoyang Beijing, 100012, China.), AK(Department of Physics and Astronomy and Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel.), AL(Department of Physics and Astronomy and Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel.), AM(South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AN(Astronomical Observatory, Jagiellonian University, Ul. Orla 171, 30-244 Cracow, Poland.; Mount Suhora Observatory, Pedagogical University, Ul. Podchorazych 2, 30-024 Cracow, Poland.), AO(Mount Suhora Observatory, Pedagogical University, Ul. Podchorazych 2, 30-024 Cracow, Poland.), AP(Mount Suhora Observatory, Pedagogical University, Ul. Podchorazych 2, 30-024 Cracow, Poland.), AQ(Observatoire Midi-Pyrénées, Université Paul Sabatier, CNRS/UMR5572, 14 Avenue Edouard Belin, 31400 Toulouse, France.), AR(Observatoire Midi-Pyrénées, Université Paul Sabatier, CNRS/UMR5572, 14 Avenue Edouard Belin, 31400 Toulouse, France.), AS(Observatoire de Paris-Meudon, DAEC, 92195 Meudon, France.), AT(School of Chemical and Physical Sciences, Victoria University of Wellington, P.O. Box 600, Wellington, New Zealand.), AU(Departamento de Física, Universidade Federal de Santa Catarina, CP 476-CEP 88040-900, Florianópolis SC, Brazil.), AV(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349.)
Publication:
The Astrophysical Journal, Volume 634, Issue 1, pp. 570-584. (ApJ Homepage)
Publication Date:
11/2005
Origin:
UCP
ApJ Keywords:
Accretion, Accretion Disks, Stars: Binaries: Close, Hydrodynamics, Stars: Novae, Cataclysmic Variables, stars: individual (DQ Her)
DOI:
10.1086/496957
Bibliographic Code:
2005ApJ...634..570W

Abstract

The old nova DQ Herculis was the Whole Earth Telescope Northern Hemisphere target for the 1997 July campaign and was observed on four nights with the SARA 0.9 m telescope during 2003 June. We present updated ephemerides for the eclipse and 71 s timings. The Fourier transform displays power at the presumed white dwarf spin period of 71.0655 s, but no significant power at either 142 or 35.5 s. The mean pulsed light curve is obtained by folding on the orbital period modulus the mean ephemeris of the 71 s period, and from this we calculate an O-C phase diagram and amplitude versus orbital phase diagrams. In addition to the phase variations during eclipse ingress and egress, the WET data reveal significant phase variations outside of eclipse. These must result from the self-eclipse of a nonaxisymmetric disk. We simulated the disk in DQ Her using smoothed particle hydrodynamics. We improve our effective spatial signal-to-noise ratio by combining 250 snapshots of the N=20,000 phase space solution over time to obtain a 5 million particle ensemble disk. From the surface shape of the ensemble disk, the radius and vertical height above the midplane of the rim of the reprocessing region can be derived as a function of azimuthal angle. From this profile we can calculate the O-C phase and amplitude diagrams as a function of inclination angle. The calculated O-C diagrams are a remarkably good match to the observed phase and amplitude variations of the 71 s signal. The best match is for inclination angle 89.7d.
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