High speed photometry of an UMa

Details High speed photometry of an UMa High speed photometry of an UMa

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985stin...8620275i&link_type=abstract

Presented at the 9th North American Workshop On Cataclysmic Variable, Seattle, Wash., 24 Jun. 1985

Physics

Cataclysmic Variables, Oscillations, Photometry, Time Dependence, Variable Stars, Power Spectra, Stellar Mass Accretion, White Dwarf Stars

Scientific paper

As a class, the AM Her objects exhibit temporal variability on time scales ranging from seconds to years. Most of the variations can be adequately described by shot noise models (Cordova and Mason 1982). Exceptions to this are the strictly periodic features modulated on the orbital periods of the systems (typically several hours) and the one to two second features which show up as excesses of power in the time averaged power spectra of AN UMa. It has been suggested that the short time scale features are due to an oscillatory instability of radiative accretion shocks discovered by Langer, Chanmugam, and Shaviv (1981, 1982). A direct physical relationship between the one to two second optical variations and shock oscillations has not yet been demonstrated. Because of the potential importance of such a result further study of these systems is clearly warranted. In this work, we examine the short time scale behavior of AN UMa in more detail and improve on the work of Middleditch (1982) by resolving the feature in time.

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