350 GeV gamma rays from AE Aqr

Bowden, C. C. G.; Bradbury, S. M.; Chadwick, P. M.; Dickinson, J. E.; Dipper, N. A.; Edwards, P. R.; Lincoln, E. W.; McComb, T. J. L.; Orford, K. J.; Rayner, S. M.; Turver, K. E.

doi:10.1016/0927-6505(92)90008-n

Cited by 42 publications

(33 citation statements)

References 8 publications

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“…A detection of TeV emission from AE Aqr has also been reported by the Durham group (Bowden et al 1992;Chadwick et al 1995 On the other hand, the analysis of data recorded by the Whipple group (68 h of observations in 1991-95) have shown no evidence for any steady, pulsed or episodic TeV emission of AE Aqr (Lang et al 1998). The upper limits to the flux of a steady emission, < ∼ 4.0 × 10 −12 cm −2 s −1 , and a pulsing emission < ∼ 1.5 × 10 −12 cm −2 s −1 , at an energy threshold of 900 GeV have been derived.…”

Section: High-energy Emissionmentioning

confidence: 85%

High-energy emission of fast rotating white dwarfs

Ikhsanov

Biermann

2005

A&A

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The process of energy release in the magnetosphere of a fast rotating, magnetized white dwarf can be explained in terms of the canonical spinpowered pulsar model. Applying this model to the white dwarf companion of the low mass close binary AE Aquarii leads us to the following conclusions. The system acts as an accelerator of charged particles whose energy is limited to E p < ∼ 3 TeV and which are ejected from the magnetosphere of the primary with the rate L kin < ∼ 10 32 erg s −1 . Due to the curvature radiation of the accelerated primary electrons the system should appear as a source of soft γ-rays (∼100 keV) with the luminosity <3 × 10 27 erg s −1 . The TeV emission of the system is dominated by the inverse Compton scattering of optical photons on the ultrarelativistic electrons. The optical photons are mainly contributed by the normal companion and the stream of material flowing through the magnetosphere of the white dwarf. The luminosity of the TeV source depends on the state of the system (flaring/quiet) and is limited to <5 × 10 29 erg s −1 . These results allow us to understand a lack of success in searching for the high-energy emission of AE Aqr with the Compton Gamma-ray Observatory and the Whipple Observatory.

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Section: High-energy Emissionmentioning

confidence: 85%

High-energy emission of fast rotating white dwarfs

Ikhsanov

Biermann

2005

A&A

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“…The bottom panel of Fig 4 shows the photocurrents of the three operational Nooitgedacht Cerenkov telescopes to confirm that the TeV burst was not the result of instrumental instability. Both these burst showed double peaked pulsed emission when folded with the P * = 33.08 s white dwarf period, implying that both poles of the rotating white dwarf is visible in VHE gamma-rays [16,18].…”

Section: Figurementioning

confidence: 99%

“…Fig. 4 and Fig 5) have been detected by both VHE gamma-ray groups [16,18]. During the night of the Nooitgedacht burst, simultaneous optical observations were made utilizing the 0.75 m telescope at SAAO.…”

Section: Figurementioning

confidence: 99%

“…respectively (e.g. [16,17,18]). Between 1988 and 1991 the Nooitgedacht Cerenkov array has observed AE Aquarii for ∼ 240 hours on moonless nights and registered ∼ 233600 Cerenkov events [17].…”

Section: Figurementioning

confidence: 99%

“…The culmination of this effect must be the white dwarf in AE Aquarii, which is probably among the most asynchronous rotators of all cataclysmic variables. Reports of Very High Energy (VHE) Gamma-ray emission (ε γ ≥ 10 11 eV) from the novalike variable AE Aquarii have been made by two independent groups (e.g [16,17,18]) in the 1990s. Unfortunately these could not be verified by more recent campaigns (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The Physics of Transient High-Energy Cosmic Sources: from Radio to VHE Gamma-rays

Meintjes¹

2016

Proceedings of XI Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF15)

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In this study magnetohydrodynamical processes that may drive particle acceleration and transient emission in the cataclysmic variables, especially the enigmatic transient multi-frequency nova-like variable, AE Aquarii, are reviewed. It is shown that the propeller ejection of material from the magnetosphere of the white dwarf may drive magnetospheric processes that can accelerate charged particles to high energies. For example, the propeller ejection of the mass transferred from the secondary star results in magnetic reconnection as well as the induction of huge field aligned potentials that may accelerate charged particles to very high energies (VHE) ε > 10 11 eV. These processes have been discussed to provide a theoretical framework to evaluate the non-thermal emission detected from this source, especially the transient burst-like VHE emission reported by two independent groups in the 1990s. In conclusion very preliminary results have been presented of a search for pulsed emission from AE Aquarii in the Fermi-LAT data.

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Simultaneous UBVRI observations of the cataclysmic variable AE Aquarii: Temperatures and masses of fireballs

et al. 2012

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We report simultaneous multicolour observations in 5 bands (U BV RI) of the flickering variability of the cataclysmic variable AE Aqr. Our aim is to estimate the parameters (colours, temperature, size) of the fireballs that produce the optical flares. The observed rise time of the optical flares is in the interval 220 -440 sec. We estimate the dereddened colours of the fireballs: (U − B)0 in the range 0.8-1.4, (B − V )0 ∼ 0.03-0.24, (V − I)0 ∼ 0.26-0.78. We find for the fireballs a temperature in the range 10000 -25000 K, mass (7-90)×10 19 g, size (3-7)×10 9 cm (using a distance of d = 86 pc). These values refer to the peak of the flares observed in U BV RI bands.

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350 GeV gamma rays from AE Aqr

Cited by 42 publications

References 8 publications

High-energy emission of fast rotating white dwarfs

High-energy emission of fast rotating white dwarfs

The Physics of Transient High-Energy Cosmic Sources: from Radio to VHE Gamma-rays

Simultaneous UBVRI observations of the cataclysmic variable AE Aquarii: Temperatures and masses of fireballs

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