A survey for QPOs in AM Herculis stars and a detailed study of the QPOs in an Ursae Majoris

Details A survey for QPOs in AM Herculis stars and a detailed study of the QPOs in an Ursae Majoris A survey for QPOs in AM Herculis stars and a detailed study of the QPOs in an Ursae Majoris

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.260..209r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 260, no. 1, p. 209-220.

Astronomy and Astrophysics

Astronomy

14

Cataclysmic Variables, Stellar Oscillations, White Dwarf Stars, Emission Spectra, Light Curve, Power Spectra, Stellar Magnetic Fields, Stellar Orbits, Stellar Spectrophotometry

Scientific paper

We have searched for quasi-periodic oscillations with frequencies between 0.1 and 2.4 Hz in the light curves of nine AM Her stars using simultaneous multi-color photometry. Oscillations were not seen in BY Cam (= H 0538 + 608), EF Eri, AM Her, DP Leo (= E 1114 + 182), ST LMi (= CW 1103 + 254), MR Ser (= PG 1550 + 191) or QQ Vul (= E 2003 + 225), but were detected in AN UMa and VV Pup. We were unable to find any systematic difference between those systems with and those without quasi-periodic oscillations. When averaged over the orbital period, the amplitude of the oscillations in AN UMa is largest in the B bandpass (about 3.5 percent). The color of the oscillations varies systematically with orbital phase, however, and the amplitude is at least as high in the U band as in the B band during the main hump in the light curve. The average coherence time as measured with autocorrelation techniques is 37 +/- 2 s for strong oscillations in the B band. We show that the accretion column is divided into 2-45 regions, each of which is oscillating simultaneously but independently. Our observations are consistent with the shock-oscillation model.

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