A Search for Radio Pulsations from AE Aquarii

Details A Search for Radio Pulsations from AE Aquarii A Search for Radio Pulsations from AE Aquarii

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...461.1016b&link_type=abstract

Astrophysical Journal v.461, p.1016

Astronomy and Astrophysics

Astronomy

9

Radio Continuum: Stars, Stars: Novae, Cataclysmic Variables, Stars: Individual Constellation Name: Ae Aquarii

Scientific paper

AE Aquarii is classified as a DQ Herculis-type cataclysmic variable, comprising a magnetized white dwarf primary and a KS dwarf secondary. Its orbital period is 9.88 hr while the rotational period of the magnetized primary is 33.08 s. AE Aqr is characterized by coherent pulsations and quasi-periodic oscillations (QPOs) in the optical, UV, and soft X-ray wavelength bands. It also emits TeV γ-rays, which may themselves be modulated on a period near the rotation period of the primary. In addition, AE Aqr displays violent flaring activity at optical, soft X-ray, and radio wavelengths.
We have searched for coherent pulsations and QPOs in the radio emission from AE Aqr. The Very Large Array (VLA) was used on 1994 January 29 to observe AE Aqr continuously for ˜10 hr at 8.4 GHz (λ = 3.6 cm). We find no evidence for the presence of coherent pulsations or QPOs. An upper limit of 1.6% of the mean flux density is placed on the amplitude of pulsations on frequencies greater than 0.01 Hz. Over bandwidths of 1% on the known fundamental and harmonic periods, the upper limits are 0.8%. The power spectrum is characterized by red noise on frequencies less than 0.01 Hz. It is well fitted by a power law with an index of 1.8. Furthermore, comparing the present observations with data obtained at seven previous epochs, we find no evidence of a relationship between flaring activity and the orbital phase.

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