The spectrum and variability of radio emission from AE Aquarii

Abada-Simon, M.; Lecacheux, A.; Bastian, T. S.; Bookbinder, Jay A.; Dulk, G. A.

doi:10.1086/172479

Cited by 52 publications

(48 citation statements)

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“…BDC have shown that the spectral index of the time averaged radio emission depends on frequency as oc v" with a = 5(2 -e)/2 if the frequency distribution of initial flux densities S 0 is given by f(S 0 ) oc So'. Abada-Simon et al 1993 have shown that the data supports a = 0.34-0.59 implying that e = 1.76-1.86. The radio spectrum of AE Aqr based on observations between 1984 and 1991 is shown in Figure 1.…”

Section: Optically Thick Synchrotron Radiationmentioning

confidence: 64%

“…The turnover frequency increases with increasing B 0 and the detection of AE Aqr at millimeter wavelengths was predicted on the basis of this model. Such radiation was indeed confirmed at frequencies up to 250 GHz on timescales of ~ 15 minutes with intensities up to 0.1 Jy, and B 0 was shown to vary between 25 and 250 G (Abada- Simon et al 1993.) BDC have shown that the spectral index of the time averaged radio emission depends on frequency as oc v" with a = 5(2 -e)/2 if the frequency distribution of initial flux densities S 0 is given by f(S 0 ) oc So'.…”

Section: Optically Thick Synchrotron Radiationmentioning

confidence: 81%

“…The solid circles and two dashed lines in the radio region indicate the range for the time-averaged radio spectra. The trapesium represents a range wherein many radio detections were reported (reproduced from Abada-Simon et al 1993.) The various infrared to ultraviolet components are also indicated by solid circles (see text).…”

Section: Introductionmentioning

confidence: 99%

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Evidence for Particle Acceleration in a Magnetized White Dwarf from Radio and Gamma-Ray Observations

Jager

1994

International Astronomical Union Colloquium

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The DQ Her-type magnetic cataclysmic variable AE Aqr contains the most rapidly spinning white dwarf (P = 33 s) in a close binary and can be considered as the "millisecond pulsar" equivalent of white dwarfs. It shows flare-like UV emission on timescales of an hour during which strong QPO activity is seen, as well as flare-like radio synchrotron emission on similar timescales up to frequencies of at least 250 GHz. It is one of the most efficient converters of accretion power to MeV electrons of all X-ray binaries, LMXB, and cataclysmic variables. TeV emission was also reported by two independent groups with a periodic and burst-like behavior similar to that seen in optical. The detection of a period derivative near 10~1 3 s/s in optical implies that the white dwarf is spinning down at a rate of ~6 X 10 33 ergs s"' which is at least an order of magnitude larger than the quiescent accretion luminosity and a few times larger than the typical UV flare luminosities. This spindown energy is not seen as disk luminosity, and the conditions appear to be favorable for the release of relativistic particles in a pulsar-type mechanism to explain the radio synchrotron emission in magnetic reconnection events, and the acceleration of particles to TeV energies in double layers if conditions are favorable.

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Section: Optically Thick Synchrotron Radiationmentioning

confidence: 64%

Section: Optically Thick Synchrotron Radiationmentioning

confidence: 81%

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Evidence for Particle Acceleration in a Magnetized White Dwarf from Radio and Gamma-Ray Observations

Jager

1994

International Astronomical Union Colloquium

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“…The radio-detected magnetic CV sample was also very small, consisting of AM Her, V834 Cen, ST Lmi, AR UMa, AE Aqr, DQ Her and BG Cmi (e.g. [32,33,34,35]). However, at the time of these discoveries there were also a large number of non-detections.…”

Section: Pos(heasa 2016)030mentioning

confidence: 99%

Cataclysmic variables: New frontiers in multi-wavelength research

Odendaal¹,

Meintjes²

2017

Proceedings of 4th Annual Conference on High Energy Astrophysics in Southern Africa — PoS(HEASA 2016)

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Compact binary systems in which a white dwarf (WD) accretes material from a non-degenerate companion, constitute some of the most prevalent, yet intriguing astronomical objects in the universe. Of special interest is a class of these binaries known as cataclysmic variables (CVs), where the transfer of material from a red dwarf companion to the WD instigates a wide range of energetic processes causing transient, variable and eruptive behaviour. These binaries, as well as a closely related class of objects known as supersoft X-ray sources (SSSs) are therefore fascinating cosmic laboratories in which the effects of fundamentally important physical phenomena like turbulence, magnetic fields, gravitation, viscosity, and particle acceleration can be studied, by modelling the observed electromagnetic radiation, from the low energy radio waves all the way up to gammaray energies. Several CVs and SSSs have been shown to exhibit high-velocity outflows, many of which are expected to be driven by magnetic fields, and modern instruments have recently shown that these outflows are associated with radio and gamma-ray emission. These developments open up an exciting new area in this field. The upcoming commissioning of MeerKAT, as well as the newly available spectropolarimetric mode on SALT, in combination with international high-energy facilities, makes this the ideal time to undertake studies of the non-thermal emission in CVs in the form of synchrotron radio emission, and non-thermal optical emission, as well as potential particle acceleration yielding high energy emission.

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“…AE Aqr reveals itself as a powerful non-thermal variable source in radio and possibly TeV γ-rays, Figure 1 [2,3,9,21], resembling the microquasar Cyg X-3 rather than any of the presently known CVs [14]. A similar radio brightness has never been observed in any of the other CVs.…”

Section: Introductionmentioning

confidence: 99%

The Peculiar Binary System AE Aquarii from its Characteristic Multi-wavelength Emission

Oruru

Meintjes

2014

EPJ Web of Conferences

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Abstract. The multi-wavelength properties of the novalike variable system AE Aquarii are discussed in terms of the interaction between the accretion inflow from a late-type main sequence star and the magnetosphere of a fast rotating white dwarf. This results in an efficient magnetospheric propeller process and particle acceleration. The spin-down of the white dwarf at a period rate of 5.64×10 −14 s s −1 results in a huge spin-down luminosity of L s−d 6×10 33 erg s −1 . Hence, the observed non-thermal hard X-ray emission and VHE and TeV gamma-ray emission may suggest that AE Aquarii can be placed in the category of spin-powered pulsars. Besides, observed hard X-ray luminosity of L X,hard ≤ 5 × 10 30 erg s −1 constitutes 0.1 % of the total spin-down luminosity of the white dwarf. This paper will discuss some recent theoretical studies and data analysis of the system.

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The spectrum and variability of radio emission from AE Aquarii

Cited by 52 publications

References 0 publications

Evidence for Particle Acceleration in a Magnetized White Dwarf from Radio and Gamma-Ray Observations

Evidence for Particle Acceleration in a Magnetized White Dwarf from Radio and Gamma-Ray Observations

Cataclysmic variables: New frontiers in multi-wavelength research

The Peculiar Binary System AE Aquarii from its Characteristic Multi-wavelength Emission

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