HS 2331+3905, the Brightest CV White Dwarf Pulsator

Details HS 2331+3905, the Brightest CV White Dwarf Pulsator HS 2331+3905, the Brightest CV White Dwarf Pulsator

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..372..597g&link_type=abstract

15th European Workshop on White Dwarfs ASP Conference Series, Vol. 372, proceedings of the conference held 7-11 August, 2006 in

Astronomy and Astrophysics

Astronomy

3

Scientific paper

We report preliminary results of infrared spectroscopy and of a multi-site photometric campaign on the brightest pulsating white dwarf in a cataclysmic variable (CV), HS 2331+3905. The Gemini J, H, and K spectra fail to reveal a clear signature of the donor star, constraining its spectral type to be L2 or later. The presence of two short-period signals at 67.62 s and 67.24 s is confirmed, and we identify the 67.62 s signal unambiguously as the white dwarf spin. Our photometric data shows that the ZZ Ceti pulsations detected near 5 min are extremely complex, with the dominant frequencies varying on time scales of hours. We suggest that the complex pulsation pattern is related to the extremely rapid rotation of the white dwarf.

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