Published in

Oxford University Press, Monthly Notices of the Royal Astronomical Society, 4(367), p. 1562-1576, 2006

DOI: 10.1111/j.1365-2966.2006.10057.x

Oxford University Press, Monthly Notices of the Royal Astronomical Society, 4(344), p. 1193-1209, 2003

DOI: 10.1046/j.1365-8711.2003.06905.x

Oxford University Press (OUP), Monthly Notices of the Royal Astronomical Society, 1(401), p. 500-506

DOI: 10.1111/j.1365-2966.2009.15666.x

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Dwarf nova oscillations and quasi-periodic oscillations in cataclysmic variables - III. A new kind of dwarf nova oscillation, and further examples of the similarities to X-ray binaries

Journal article published in 2003 by Brian Warner, Patrick A. Woudt ORCID, Magaretha L. Pretorius
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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Abstract

We present new observations of the rapid oscillations in the dwarf nova VW Hyi, made late in outburst. These dwarf nova oscillations (DNOs) increase in period until they reach 33 s, when a transition to a strong 1st harmonic and weak fundamental takes place. After further period increase the 2nd harmonic appears; often all three components are present simultaneously. This 1:2:3 frequency suite is similar to what has been seen in some neutron star and black hole X-Ray binaries, but has not previously been seen in a cataclysmic variable. When studied in detail the fundamental and 2nd harmonic vary similarly in phase, but the 1st harmonic behaves independently, though keeping close to twice the frequency of the fundamental. The fundamental period of the DNOs, as directly observed or inferred from the harmonics, increases to ~100 s before the oscillation disappears as the star reaches quiescence. Its maximum period is close to that of the `longer period' DNOs observed in VW Hyi. The quasi-periodic oscillations (QPOs), which have fundamental periods 400 -- 1000 s, behave in the same way, showing 1st and 2nd harmonics at approximately the same times as the DNOs. We explore some possible models. One in which the existence of the 1st harmonic is due to transition from viewing a single accretion region to viewing two regions, and the rate of accretion onto the primary is modulated at the frequency of the 1st harmonic, as in the `beat frequency model', can generate the suite of DNO frequencies observed. But the behaviour of the QPOs is not yet understood. Comment: 16 pages, 13 figures; accepted for publication in MNRAS