AM CVn - Finally solved? Results of XCOV4, March 1990

Details AM CVn - Finally solved? Results of XCOV4, March 1990 AM CVn - Finally solved? Results of XCOV4, March 1990

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993balta...2..459s&link_type=abstract

Baltic Astronomy, vol. 2, p. 459

Astronomy and Astrophysics

Astronomy

1

Cataclysmic Variables, Stellar Oscillations, Dwarf Stars, Ubv Spectra, Light Curve

Scientific paper

Preliminary results of the analysis of the XCOV4 campaign data in March and April 1990 for AM CVn are presented. The pulse spectrum has five harmonics of the undetected fundamental period 1051 s. In addition, sidebands are observed with a 21 microHz spacing, always on the high-frequency side. It is not possible to explain these observations as g-mode pulsations. Most likely, AM CVn is a system of two interacting dwarf stars transferring mass through an elliptical disk slightly tilted with respect to the orbital plane. The disk has a retrograde precession with a period of 13.4 h, resulting in the 21 microHz side bands observed. We interpret the 1051 s fundamental period as the superhump period and 1028 s as the orbital period, while 1011 s is a beat period of a prograde precession of the disk with a period of 17 h. The 13.4 h period is also detected in variations of the absorption line profiles, proving that this period represents a disk phenomenon.

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