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Title:
Superhumps in Cataclysmic Binaries. XXIII. V442 Ophiuchi and RX J1643.7+3402
Authors:
Patterson, Joseph; Fenton, William H.; Thorstensen, John R.; Harvey, David A.; Skillman, David R.; Fried, Robert E.; Monard, Berto; O'Donoghue, Darragh; Beshore, Edward; Martin, Brian; Niarchos, Panos; Vanmunster, Tonny; Foote, Jerry; Bolt, Greg; Rea, Robert; Cook, Lewis M.; Butterworth, Neil; Wood, Matt
Affiliation:
AA(Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027; .; Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation.), AB(Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755; , .), AC(Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755; , .), AD(Center for Backyard Astrophysics (West), 1552 West Chapala Drive, Tucson, AZ 85704; .), AE(Center for Backyard Astrophysics (East), 9517 Washington Avenue, Laurel, MD 20723; .), AF(Center for Backyard Astrophysics (Flagstaff), Braeside Observatory, P.O. 906, Flagstaff, AZ 86002; .), AG(Center for Backyard Astrophysics (Pretoria), P.O. 70284, Die Wilgers 0041, Pretoria, South Africa; .), AH(South African Astronomical Observatory, Observatory 7935, Cape Town, South Africa; .), AI(Center for Backyard Astrophysics (Colorado), 14795 East Coachman Drive, Colorado Springs, CO 80908; .), AJ(King's University College, Department of Physics, 9125 50th Street, Edmonton, AB T5H 2M1, Canada; .), AK(University of Athens, Department of Astrophysics, Astronomy, and Mechanics, Panepistimipolis, GR-157 84, Zografos, Athens, Greece; .), AL(Center for Backyard Astrophysics (Belgium), Walhostraat 1A, B-3401 Landen, Belgium; .), AM(Center for Backyard Astrophysics (Utah), 4175 East Red Cliffs Drive, Kanab, UT 84741; .), AN(Center for Backyard Astrophysics (Perth), 295 Camberwarra Drive, Craigie, Western Australia 6025, Australia; .), AO(Center for Backyard Astrophysics (Nelson), 8 Regent Lane, Richmond, Nelson, New Zealand; .), AP(Center for Backyard Astrophysics (Concord), 1730 Helix Court, Concord, CA 94518; .), AQ(Center for Backyard Astrophysics (Townsville), 24 Payne Street, Mount Louisa, Queensland 4814, Australia; .), AR(Florida Institute of Technology, Department of Physical and Space Sciences and SARA Observatory, Melbourne, FL 32901; .)
Publication:
The Publications of the Astronomical Society of the Pacific, Volume 114, Issue 802, pp. 1364-1381. (PASP Homepage)
Publication Date:
12/2002
Origin:
UCP
PASP Keywords:
accretion, accretion disks, Stars: Binaries: Close, Stars: Novae, Cataclysmic Variables, stars: individual (V442 Ophiuchi), stars: individual (RX J1643.7+3402)
DOI:
10.1086/344587
Bibliographic Code:
2002PASP..114.1364P

Abstract

We report the results of long observing campaigns on two novalike variables: V442 Ophiuchi and RX J1643.7+3402. These stars have high-excitation spectra, complex line profiles signifying mass loss at particular orbital phases, and similar orbital periods (respectively, 0.12433 and 0.12056 days). They are well-credentialed members of the SW Sex class of cataclysmic variables. Their light curves are also quite complex. V442 Oph shows periodic signals with periods of 0.12090(8) and 4.37(15) days, and RX J1643.7+3402 shows similar signals at 0.11696(8) and 4.05(12) days. We interpret these short and long periods, respectively, as a ``negative superhump'' and the wobble period of the accretion disk. The superhump could then possibly arise from the heating of the secondary (and structures fixed in the orbital frame) by inner-disk radiation, which reaches the secondary relatively unimpeded since the disk is not coplanar. At higher frequencies, both stars show another type of variability: quasi-periodic oscillations with a period near 1000 s. Underlying these strong signals of low stability may be weak signals of higher stability. Similar quasi-periodic oscillations, and negative superhumps, are quite common features in SW Sex stars. Both can in principle be explained by ascribing strong magnetism to the white dwarf member of the binary; and we suggest that SW Sex stars are borderline AM Herculis binaries, usually drowned by a high accretion rate. This would provide an ancestor channel for AM Hers, whose origin is still mysterious.
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