A Study of the X‐Ray Emission of the Magnetic Cataclysmic Variable AE Aquarii

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Abstract
We report results from analysis of the X-ray observations of AE Aqr, made with Ginga in 1988 June and with ASCA in 1995 October. Pulsations are detected clearly with a sinusoidal pulse profile with periods of 33.076 ± 0.001 s (Ginga) and 33.077 ± 0.003 s (ASCA). The pulse amplitude is relatively small, and the modulated flux remains nearly constant despite a factor of 3 change in the average flux during the flare. We reproduce the time-averaged spectrum in the 0.4-10 keV energy band by a thermal emission model with a combination of two different temperatures: kT1 = 0.68 keV and kT2 = 2.9 keV. There is no significant difference between the quiescent and flare energy spectra, although a hint of spectral hardening is recognized during the flare. We interpret these observational results with a model in which AE Aqr is in a propeller stage. Based on this propeller scenario, we suggest that the X-ray emission originates from magnetospheric radiation.
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