High-Speed Photometry of AM CVn Stars

Details High-Speed Photometry of AM CVn Stars High-Speed Photometry of AM CVn Stars

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..797..287w&link_type=abstract

INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP Conference Proceedings, Volume 797, pp. 287-294 (2005).

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Cataclysmic Binary Stars, Stellar Photometry, Oscillations, Cataclysmic Binaries, Symbiotic Stars, Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Photography And Photometry

Scientific paper

We present high-speed photometry of three AM CVn stars discovered in the last few years (ES Cet, `2003aw' and SDSS J1240). ES Cet has a very stable photometric modulation with a single period of 620.2117 (+/- 0.0002) s (Espaillat et al. 2005) which is identical to its spectroscopic period. The 2-sigma upper limit on the period derivative (Ṗ) of ES Cet is < 1.5 × 10-11, based on a 3-year observational baseline. Since the discovery of `2003aw' in a supernova search, this AM CVn star has been observed during two outbursts and has a superhump modulation of Psh = 2041.5 +/- 0.3 s. At quiescence, 2003aw is fairly faint (V ~ 20.4 mag) and no orbital period has yet been derived for this system. Two of the AM CVn stars (V803 Cen and CR Boo) show rapid oscillations similar to the (longer-period) dwarf nova oscillations and quasi-periodic oscillations seen in hydrogen-rich high-Ṁ CVs (Warner 2004).

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