Influence of multiple scattering on the radiation of relativistic particles in amorphous and crystalline media

Akhiezer, A.I.; Шульга, Н.Ф.

doi:10.1070/pu1987v030n03abeh002818

Cited by 52 publications

(29 citation statements)

References 15 publications

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“…The character of the emission depends crucially on the "formation" or "coherence" length of the radiated photons Akhiezer & Shul'ga (1987). At low frequencies, this length becomes large, but we confine our estimates to the highest frequency photons produced in the interaction.…”

Section: Radiative Signaturesmentioning

confidence: 99%

Radiative Signatures of Relativistic Shocks

Kirk

Reville

2010

ApJ

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Particle-in-cell simulations of relativistic, weakly magnetized collisionless shocks show that particles can gain energy by repeatedly crossing the shock front. This requires scattering off self-generated small length-scale magnetic fluctuations. The radiative signature of this first-order Fermi acceleration mechanism is important for models of both the prompt and afterglow emission in gamma-ray bursts and depends on the strength parameter a = λe|δB|/mc 2 of the fluctuations (λ is the length scale and |δB| is the magnitude of the fluctuations). For electrons (and positrons), acceleration saturates when the radiative losses produced by the scattering cannot be compensated by the energy gained on crossing the shock. We show that this sets an upper limit on both the electron Lorentz factor γ < 10 6 (n/1 cm −3 ) −1/6γ 1/6 and on the energy of the photons radiated during the scattering process hω max < 40 Max(a, 1)(n/1 cm −3 ) 1/6γ −1/6 eV, where n is the number density of the plasma andγ is the thermal Lorentz factor of the downstream plasma, provided a < a crit ∼ 10 6 . This rules out "jitter" radiation on self-excited fluctuations with a < 1 as a source of gamma rays, although high-energy photons might still be produced when the jitter photons are upscattered in an analog of the synchrotron self-Compton process. In fluctuations with a > 1, radiation is generated by the standard synchrotron mechanism, and the maximum photon energy rises linearly with a, until saturating at 70 MeV, when a = a crit .

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Section: Radiative Signaturesmentioning

confidence: 99%

Radiative Signatures of Relativistic Shocks

Kirk

Reville

2010

ApJ

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“…In the classical electrodynamics coherent length is the distance over which constructive interference between radiated waves takes place. During the time the electron travels the formation length it and the radiated electromagnetic wave separate enough [14] to be considered independent particles. In bremsstrahlung this separation is at least a distance of the order of the emitted photon wavelength λ.…”

Section: Formation Length and LI Violationmentioning

confidence: 99%

Lorentz invariance violation and the QED formation length

Vankov

Stanev

2002

Physics Letters B

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It was recently suggested that possible small violations of Lorentz invariance could explain the existence of UHECR beyond the GZK cutoff and the observations of multi-TeV gamma-rays from Mkn 501. Our analysis of Lorentz-violating kinematics shows that in addition to the modified threshold conditions solving cosmic ray puzzles we should expect a strong suppression of electromagnetic processes like bremsstrahlung and pair creation. This leads to drastic effects in electron-photon cascade development in the atmosphere and in detectors.

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“…Moreover, even for an interaction with one SLSW, there are ambiguous points in the consideration of the typical frequency. To estimate the typical frequency of the radiation, we have to know the photon formation time (Akhiezer & Shul'ga 1987, Reville & Kirk 2010, which is the inverse of the cyclotron frequency mc/eB in the context of synchrotron radiation. Previous studies considered cases for which the phase-locking effect is weak, which means that the velocity is oblique to the wavevector direction.…”

Section: Introductionmentioning

confidence: 99%

Particle Acceleration in Superluminal Strong Waves

Teraki

Ito

Nagataki

2015

ApJ

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We calculate the electron acceleration in random superluminal strong waves (SLSWs) and radiation from them using numerical methods in the context of the termination shocks of pulsar wind nebulae. We pursue the orbit of electrons by solving the equation of motion in the analytically expressed electromagnetic turbulences. These consist of a primary SLS and isotropically distributed secondary electromagnetic waves. Under the dominance of the secondary waves, all electrons gain nearly equal energy. On the other hand, when the primary wave is dominant, selective acceleration occurs. The phase of the primary wave for electrons moving nearly along the wavevector changes very slowly compared with the oscillation of the wave, which is "phase-locked," and such electrons are continuously accelerated. This acceleration by SLSWs may play a crucial role in pre-shock acceleration. In general, the radiation from the phase-locked population is different from the synchro-Compton radiation. However, when the amplitude of the secondary waves is not extremely weaker than that of the primary wave, the typical frequency can be estimated from synchro-Compton theory using the secondary waves. The primary wave does not contribute to the radiation because the SLSW accelerates electrons almost linearly. This radiation can be observed as a radio knot at the upstream of the termination shocks of the pulsar wind nebulae without counterparts in higher frequency ranges.

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Influence of multiple scattering on the radiation of relativistic particles in amorphous and crystalline media

Abstract: The dissociative recombination rate coefficient for CO + has been measured at 300 K using a flowing afterglow Langmuir probe-mass spectrometer apparatus. A value of (1.85 ± 0.5) × 10 −7 cm 3 s −1 has been found.

Cited by 52 publications

References 15 publications

Radiative Signatures of Relativistic Shocks

Radiative Signatures of Relativistic Shocks

Lorentz invariance violation and the QED formation length

Particle Acceleration in Superluminal Strong Waves

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