Particle kinetics in highly turbulent plasmas (renormalization and self-consistent field methods)

Bykov, A. M.; Топтыгин, И. Н.

doi:10.1070/pu1993v036n11abeh002179

Cited by 109 publications

(102 citation statements)

References 4 publications

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“…The composite spectrum of cosmic rays from an ensemble of shocks in a supersonically turbulent medium was determined by Schneider (1993). In such a medium, the summed energy distribution for cosmic rays from all of the shocks is close to a power law, but there can be flat parts or bumps, unlike the energy distribution from a single shock (see also Achterberg 1990, Bykov & Toptygin 1993.…”

Section: Other Scattering Mechanismsmentioning

confidence: 99%

Interstellar Turbulence II: Implications and Effects

Scalo

Elmegreen

2004

Annu. Rev. Astron. Astrophys.

309

157

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Interstellar turbulence has implications for the dispersal and mixing of the elements, cloud chemistry, cosmic ray scattering, and radio wave propagation through the ionized medium. This review discusses the observations and theory of these effects. Metallicity fluctuations are summarized, and the theory of turbulent transport of passive tracers is reviewed. Modeling methods, turbulent concentration of dust grains, and the turbulent washout of radial abundance gradients are discussed. Interstellar chemistry is affected by turbulent transport of various species between environments with different physical properties and by turbulent heating in shocks, vortical dissipation regions, and local regions of enhanced ambipolar diffusion. Cosmic rays are scattered and accelerated in turbulent magnetic waves and shocks, and they generate turbulence on the scale of their gyroradii. Radio wave scintillation is an important diagnostic for small scale turbulence in the ionized medium, giving information about the power spectrum and amplitude of fluctuations. The theory of diffraction and refraction is reviewed, as are the main observations and scintillation regions.

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Section: Other Scattering Mechanismsmentioning

confidence: 99%

Interstellar Turbulence II: Implications and Effects

Scalo

Elmegreen

2004

Annu. Rev. Astron. Astrophys.

309

157

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“…The inclusion of perpendicular diffusion with κ = 0.02κ ⊥ does not change the growth rate noticeably. It should be noted however, that the turbulent advection due to magnetic fluctuations of scales larger than the CR mean free path would make the diffusion coefficient nearly isotropic on scales interesting for the Parker instability (see Bykov and Toptygin 1993). A non-linear development of Parker instability was simulated by Kuwabara et al (2004).…”

Section: Instabilities and Plasma Effectsmentioning

confidence: 99%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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We briefly review sources of cosmic rays, their composition and spectra as well as their propagation in the galactic and extragalactic magnetic fields, both regular and fluctuating. A special attention is paid to the recent results of the X-ray and gamma-ray observations that shed light on the origin of the galactic cosmic rays and the challenging results of Pierre Auger Observatory on the ultra high energy cosmic rays. The perspectives of both high energy astrophysics and cosmic-ray astronomy to identify the sources of ultra high energy cosmic rays, the mechanisms of particle acceleration, to measure the intergalactic radiation fields and to reveal the structure of magnetic fields of very different scales are outlined.

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“…The corresponding energy E 1 that separates different regimes can be estimated from the condition ψ ∼ 1 or l D (E 1 ) ∼ l sh which for the conditions of the Fermi bubble is In the case of ψ 1 or l sh l D analyzed in Bykov & Toptygin [11], Bykov & Fleishman [10], there is a combined effect of a fast particle acceleration by a single shock, which generates the spectrum E −2 and relatively slow transformation of this spectrum due to interaction with other shocks (stochastic Fermi acceleration) into a hard E −1 spectrum in the intershock medium at relatively low energies. However it is unclear if such slow transformation can be completed within the life time of the shocks in the Bubble.…”

Section: Reacceleration Of the Hadronic Component Of Cr By Fermi Bubblesmentioning

confidence: 99%

Fermi bubbles as a source of cosmic rays above 1015 eV

Chernyshov

Cheng

Dogiel

et al. 2014

Nuclear Physics B - Proceedings Supplements

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Fermi bubbles are giant gamma-ray structures extended north and south of the Galactic center with characteristic sizes of order of 10 kpc recently discovered by Fermi Large Area Telescope. Good correlation between radio and gamma-ray emission in the region covered by Fermi bubbles implies the presence of high-energy electrons in this region. Since it is relatively difficult for relativistic electrons of this energy to travel all the way from the Galactic sources toward Fermi bubbles one can assume that they accelerated in-situ. The corresponding acceleration mechanism should also affect the distribution of the relativistic protons in the Galaxy. Since protons have much larger lifetimes the effect may even be observed near the Earth. In our model we suggest that Fermi bubbles are created by acceleration of electrons on series of shocks born due to periodic star accretions by supermassive black hole Sgr A*. We propose that hadronic CR within the "knee" of the observed CR spectrum are produced by Galactic supernova remnants distributed in the Galactic disk. Reacceleration of these particles in the Fermi Bubble produces CRs beyond the knee. This model provides a natural explanation of the observed CR flux, spectral indexes, and matching of spectra at the knee.

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Particle kinetics in highly turbulent plasmas (renormalization and self-consistent field methods)

Cited by 109 publications

References 4 publications

Interstellar Turbulence II: Implications and Effects

Interstellar Turbulence II: Implications and Effects

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Fermi bubbles as a source of cosmic rays above 1015 eV

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