The unusual helium variable AM Canum Venaticorum

Abstract

The unusual variable star AM CVn has puzzled astronomers for over 40 years. This object, both a photometric and spectroscopic variable, is believed to contain a pair of hydrogen-deficient white dwarfs of extreme mass ratio, transferring material via an accretion disk. We examine the photometric properties of AM CVn, analyzing 289 hours of high-speed photometric data spanning 1976 to 1992. The power spectrum displays significant peaks at 988.7, 1248.8, 1902.5, 2853.8, 3805.2, 4756.5, and 5707.8 μHz (1011.4, 800.8, 525.6, 350.4, 262.8, 210.2, and 175.2 s). We find no detectable power at 951.3 μHz (1051 s), the previously reported main frequency. The 1902.5, 2853.9, and 3805.2 μHz peaks are multiplets, with frequency splitting in each case of 20.77 ± 0.05 μHz. The 1902.5 μHz seasonal pulse shapes are identical, within measurement noise, and maintain the same amplitude and phase as a function of color. We have determined the dominant frequency to be 1902.509802 ± 0.00001 μHz, with p = + 1.71 (±0.04) X 10-11 s s-ˡ. We discuss the implications of these findings on a model forAM CVn