Abstract
High speed photometry of the helium-transferring binary ES Cet — taken over a two-year period (2001 October – 2003 October) — shows a very stable photometric period of 620.211437 ± 0.000038 s, with a tentative indication of curvature in the O-C diagram suggesting a change in period at a rate of \(\dot P \sim 1.6 \times 10^{ - 11} \). Phase-resolved spectroscopy of ES Cet obtained with the Hobby-Eberly Telescope shows a clear modulation on the photometric period, the assumed orbital period. We have followed a newly identified AM CVn star (‘2003aw’) photometricaly through its 2003 February/March outburst during which it varied in brightness over a range of V = 16.5 – 20.3; we find a superhump period of 2041.5 ± 0.3 s. Questions are raised about the reality of the detected spin-up in RX J0806 (Hakala et al. 2003; Strohmayer 2003).
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Woudt, P.A., Warner, B. (2005). AM CVn Stars in the UCT CCD CV Survey. In: Sion, E.M., Vennes, S., Shipman, H.L. (eds) White Dwarfs: Cosmological and Galactic Probes. Astrophysics and Space Science Library, vol 332. Springer, Dordrecht. https://doi.org/10.1007/1-4020-3725-2_22
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