The unusual helium variable AM Canum Venaticorum

Details The unusual helium variable AM Canum Venaticorum The unusual helium variable AM Canum Venaticorum

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...445..927p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 445, no. 2, p. 927-938

Astronomy and Astrophysics

Astrophysics

32

Accretion Disks, B Stars, Stellar Atmospheres, Stellar Models, Stellar Oscillations, Variable Stars, White Dwarf Stars, Absorption Spectra, Data Reduction, Mass Transfer, Stellar Color, Stellar Evolution, Stellar Structure

Scientific paper

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 microHz (1011.4, 800.8, 525.6, 350.4, 262.8, 210.2, and 175.2 s). We find no detectable power at 951.3 microHz (1051 s), the previously reported main frequency. The 1902.5, 2853.9, and 3805.2 microHz peaks are multiplets, with frequency splitting in each case of 20.77 +/- 0.05 microHz. The 1902.5 microHz 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 1902.50902 +/- 0.00001 microHz with dot P = +1.71 (+/- 0.04) x 10-11 s/s. We discuss the implications of these findings on a model for AM CVn.

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