Analysis of the oscillations in HST observations of the quiescent SU UMa type dwarf nova WZ Sagittae |
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| Authors: | Warren Skidmore William F Welsh Janet H Wood M S Catalán Keith Horne |
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| Institution: | Department of Physics, Keele University, Keele, Staffordshire ST5 5BG; School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS; Physics and Astronomy Department, University of Wyoming, WY 82071, USA; Department of Astronomy, University of Texas, Austin, TX 78712, USA |
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| Abstract: | An analysis of the UV oscillations in WZ Sge is presented, in which we obtain the oscillation amplitude spectra. We find a strong 27.9-s oscillation in our Hubble Space Telescope ( HST ) UV and zeroth-order light curves as well as weaker oscillations at 28.4 s in the UV and 29.1 s in the zeroth order. We find that the main oscillation amplitude spectrum can be fitted with static white dwarf spectra of about 17 000 K, an accretion hotspot of only a few 100 K hotter than the underlying white dwarf temperature or a variety of cool (<14 500 K) white dwarf pulsation amplitude spectra. A pulsating white dwarf can also explain the very blue colour of oscillations of different periods previously found in the optical. Comparing our results with those of Welsh et al., we see that the amplitude spectra of the main oscillations in WZ Sge measured with different periods in data sets from different epochs are similar to each other. Our results raise questions about using the magnetically accreting rotating white dwarf model to explain the oscillations. We suggest that the pulsating white dwarf model is still a viable explanation for the oscillations in WZ Sge. |
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| Keywords: | binaries: general stars: individual: WZ Sge novae cataclysmic variables stars: oscillations |
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