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A 16-yr photometric campaign on the eclipsing novalike variable DW Ursae Majoris
Boyd, D. R. S.; de Miguel, E.; Patterson, J.; Wood, M. A.; Barrett, D.; Boardman, J.; Brettman, O.; Cejudo, D.; Collins, D.; Cook, L. M.; Cook, M. J.; Foote, J. L.; Fried, R.; Gomez, T. L.; Hambsch, F.-J.; Jones, J. L.; Kemp, J.; Koff, R.; Koppelman, M.; Krajci, T.; Lemay, D.; Martin, B.; McClusky, J. V.; Menzies, K.; Messier, D.; Roberts, G.; Robertson, J.; Rock, J.; Sabo, R.; Skillman, D.; Ulowetz, J.; Vanmunster, T.
AA(CBA Oxford, West Challow Observatory, 5 Silver Lane, West Challow OX12 9TX, UK), AB(Departamento de Ciencias Integradas, Facultad de Ciencias Experimentales, Universidad de Huelva, E-21071 Huelva, Spain; CBA Huelva, Observatorio del CIECEM, Parque Dunar, Matalascañas, E-21760 Almonte, Huelva, Spain), AC(Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA), AD(Department of Physics and Astronomy, Texas A&M University-Commerce, Commerce, TX 75429, USA), AE(Observatory Le Marouzeau, 6 Le Marouzeau, St Leger Bridereix F-23300, France), AF(CBA Wisconsin, Luckydog Observatory, 65027 Howath Road, de Soto, WI 54624, USA), AG(CBA Huntley, 13915 Hemmingsen Road, Huntley, IL 60142, USA), AH(CBA Madrid, Observatorio El gallinero, El Berrueco, E-28192 Madrid, Spain), AI(College View Observatory, 138 College View Drive, Swannanoa, NC 28778, USA), AJ(CBA Concord, 1730 Helix Court, Concord, CA 94518, USA), AK(CBA Ontario, Newcastle Observatory, 9 Laking Drive, Newcastle, ON L1B 1M5, Canada), AL(CBA Utah, 4175 E. Red Cliffs Drive, Kanab, UT 84741, USA), AM(Braeside Observatory, Flagstaff, AZ 86002, USA), AN(Instituto de Ciencias Matemáticas, Campus de Cantoblanco UAM, E-28049 Madrid, Spain; CBA Cuenca, E-16540 Bonilla, Cuenca, Spain), AO(CBA Mol, Andromeda Observatory, Oude Bleken 12, B-2400 Mol, Belgium), AP(CBA Oregon, 22665 Bents Road NE, Aurora, OR 97002, USA), AQ(Department of Physics, Middlebury College, Middlebury, VT 05753, USA), AR(CBA Colorado, Antelope Hills Observatory, 980 Antelope Drive West, Bennett, CO 80102, USA), AS(6019 Fairwood Drive, Minnetonka, MN 55345, USA), AT(CBA New Mexico, PO Box 1351 Cloudcroft, NM 88317, USA), AU(CBA Quebec, 195 Rang 4 Ouest, St-Anaclet, QC, G0K 1H0, Canada), AV(CBA Alberta, Department of Physics, King's University College, 9125 50th Street, Edmonton, AB T5H 2M1, Canada), AW(Blackburn College, 700 College Ave., Carlinville, IL 62626, USA), AX(CBA Massachusetts, 318A Potter Road, Framingham, MA 01701, USA), AY(CBA Norwich, 35 Sergeants Way, Lisbon, CT 06351, USA), AZ(CBA Tennessee, 2007 Cedarmont Drive, Franklin, TN 37067, USA), BA(Department of Physical Science, Arkansas Tech University, 1701 North Boulder Avenue, Russellville, AR 72801, USA), BB(CBA Wilts, 2 Spa Close, Highworth, Swindon, SN6 7PJ, UK), BC(CBA Montana, 2336 Trailcrest Drive, Bozeman, MT 59718, USA), BD(CBA Mountain Meadows, 6-G Ridge Road, Greenbelt, MD 20770, USA), BE(CBA Illinois, Northbrook Meadow Observatory, 855 Fair Lane, Northbrook, IL 60062, USA), BF(CBA Belgium, Walhostraat 1A, B-3401 Landen, Belgium)
Monthly Notices of the Royal Astronomical Society, Volume 466, Issue 3, p.3417-3433 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
accretion, accretion discs, binaries: eclipsing, stars: individual: DW Ursae Majoris, novae, cataclysmic variables, white dwarfs
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


We present an analysis of photometric observations of the eclipsing novalike variable DW UMa made by the CBA consortium between 1999 and 2015. Analysis of 372 new and 260 previously published eclipse timings reveals a 13.6 yr period or quasi-period in the times of minimum light. The seasonal light curves show a complex spectrum of periodic signals: both positive and negative 'superhumps', likely arising from a prograde apsidal precession and a retrograde nodal precession of the accretion disc. These signals appear most prominently and famously as sidebands of the orbital frequency; but the precession frequencies themselves, at 0.40 and 0.22 cycles per day, are also seen directly in the power spectrum. The superhumps are sometimes seen together, and sometimes separately. The depth, width and skew of eclipses are all modulated in phase with both nodal and apsidal precession of the tilted and eccentric accretion disc. The superhumps, or more correctly the precessional motions that produce them, may be essential to understanding the mysterious 'SW Sextantis' syndrome. Disc wobble and eccentricity can both produce Doppler signatures inconsistent with the true dynamical motions in the binary, and disc wobble might boost the mass-transfer rate by enabling the hot white dwarf to directly irradiate the secondary star.
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