Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.1507m&link_type=abstract
American Astronomical Society, AAS Meeting #212, #15.07; Bulletin of the American Astronomical Society, Vol. 40, p.530
Astronomy and Astrophysics
Astronomy
Scientific paper
Accreting white dwarfs in cataclysmic variables (CVs) have also recently been shown to exhibit non-radial pulsations similar to their non-interacting counterparts; GW Librae was the first accreting pulsator discovered in 1998 (Warner & van Zyl 1998; van Zyl et al. 2000, 2004). When the orbital period of a CV is close to the evolutionary period minimum, the accretion rate is small (Gaensicke et al. 2006). The system is in quiescence and the white dwarf flux dominates the light from the CV (Sion 1999). A search for non-radial pulsations among suitable candidates close to the period minimum has led to the discovery of 12 such systems known to date. These unique systems provide us with an opportunity to learn about the physical parameters of the accreting and pulsating white dwarf using the technique of asteroseismology.
Accreting pulsators are of interest as they have likely undergone a few billion years of accretion and thousands of thermonuclear runaways. Questions we can address by studying these systems will be to what extent accretion affects the white dwarf mass, temperature, and composition and how efficiently angular momentum is transferred into the core of the white dwarf. Accreting pulsators in non-eclipsing CVs may prove to be our only opportunity to obtain meaningful mass constraints for the primary white dwarfs. Constraining the population, mass distribution, and evolution of accreting white dwarfs is also important for studying supernovae Type Ia systematics.
We present the results from our multi-site observations of the accreting white dwarf pulsator SDSSJ161033.64-010223.3 (Woudt & Warner 2004), acquired in May 2007. The pulsation spectrum shows two independent periods at 609s and 347s. The light curve also allows us to measure the orbital period of the pulsating white dwarf using two different methods. We thank NSF for partial support of this project through the grant AST-0607840.
Bildsten Lars
Gaensicke Boris
Mukadam Anjum Shagufta
Sion Edward M.
Szkody Paula
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