Analysis of the oscillations in HST observations of the quiescent SU UMa type dwarf nova WZ Sagittae

Details Analysis of the oscillations in HST observations of the quiescent SU UMa type dwarf nova WZ Sagittae Analysis of the oscillations in HST observations of the quiescent SU UMa type dwarf nova WZ Sagittae

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.310..750s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 310, Issue 3, pp. 750-758.

Astronomy and Astrophysics

Astronomy

12

Binaries: General, Stars: Individual: Wz Sge, Novae, Cataclysmic Variables, Stars: Oscillations

Scientific paper

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 28.4s in the UV and 29.1s in the zeroth order. We find that the main oscillation amplitude spectrum can be fitted with static white dwarf spectra of about 17000K, an accretion hotspot of only a few 100K hotter than the underlying white dwarf temperature or a variety of cool (<14500K) 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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