Propagation of a fast electron cloud in a solar-like plasma of decreasing density

Kontar, Eduard P.

doi:10.1088/0741-3335/43/4/314

Cited by 18 publications

(9 citation statements)

References 22 publications

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“…The asymptotic (long time) solution to the quasi-linear equations is thus a plateau in velocity space (e.g. Vedenov & Ryutov, 1972;Grognard, 1985;Kontar, 2001c). Figure 6 shows an example of the resonant interaction of Langmuir waves with electrons, and the resulting quasi-linear relaxation.…”

Section: Writing the Electron Distribution Function As F (V T) [Elecmentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

335

217

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Solar type III radio bursts are an important diagnostic tool in the understanding of solar accelerated electron beams. They are a signature of propagating beams of nonthermal electrons in the solar atmosphere and the solar system. Consequently, they provide information on electron acceleration and transport, and the conditions of the background ambient plasma they travel through. We review the observational properties of type III bursts with an emphasis on recent results and how each property can help identify attributes of electron beams and the ambient background plasma. We also review some of the theoretical aspects of type III radio bursts and cover a number of numerical efforts that simulate electron beam transport through the solar corona and the heliosphere.

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Section: Writing the Electron Distribution Function As F (V T) [Elecmentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

335

217

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“…Later, however, the issue was resolved in the context of the finite physical dimension of the source size, which leads to the beam-reformation via the time-of-flight effects. Thus, the propagation and relaxation of type III electrons either in homogeneous and inhomogeneous media, with or without the effects of finite source size, i.e., the time-of-flight effects, together with the excitation and saturation of Langmuir turbulence, have received extensive discussions in the literature (Sturrock 1964;Zheleznyakov & Zaitsev 1970b;Zaitsev et al 1972;Papadopoulos et al 1974Papadopoulos et al , 1975Takakura & Shibahashi 1976;Magelssen & Smith 1977;Goldstein et al 1979;Smith et al 1979;Grognard 1980Grognard , 1982Grognard , 1985Muschietti 1990;Mel'nik et al 1999;Kontar 2001aKontar , 2001bKontar , 2001cKontar & Pécsely 2002;Ziebell et al 2001Ziebell et al , 2008aZiebell et al , 2008bZiebell et al , 2012Ziebell et al , 2014aZiebell et al , 2014bZiebell et al , 2014cLi et al 2003Li et al , 2005aLi et al , 2005bLi et al , 2006aLi et al , 2006bLi et al , 2006cLi et al , 2008aLi et al , 2008bLi et al , 2009Li et al , 2010Li et al , 2011aLi et al , 2011bLi et al , 2011c…”

Section: Case Studymentioning

confidence: 99%

Plasma Emission by Nonlinear Electromagnetic Processes

Ziebell

Yoon

Petruzzellis

et al. 2015

ApJ

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The plasma emission, or electromagnetic (EM) radiation at the plasma frequency and/or its harmonic(s), is generally accepted as the radiation mechanism responsible for solar type II and III radio bursts. Identification and characterization of these solar radio burst phenomena were done in the 1950s. Despite many decades of theoretical research since then, a rigorous demonstration of the plasma emission process based upon first principles was not available until recently, when, in a recent Letter, Ziebell et al. reported the first complete numerical solution of EM weak turbulence equations; thus, quantitatively analyzing the plasma emission process starting from the initial electron beam and the associated beam-plasma (or Langmuir wave) instability, as well as the subsequent nonlinear conversion of electrostatic Langmuir turbulence into EM radiation. In the present paper, the same problem is revisited in order to elucidate the detailed physical mechanisms that could not be reported in the brief Letter format. Findings from the present paper may be useful for interpreting observations and full-particle numerical simulations.

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“…Due to this shift we have more waves with low phase velocity than the electrons are able to absorb at the back. As a result the low velocity waves form a "trace" of the structure (Kontar 2001).…”

Section: The Energy Distribution Of Wavesmentioning

confidence: 99%

Dynamics of electron beams in the solar corona plasma with density fluctuations

Kontar¹

2001

A&A

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Abstract. The problem of beam propagation in a plasma with small scale and low intensity inhomogeneities is investigated. It is shown that the electron beam propagates in a plasma as a beam-plasma structure and is a source of Langmuir waves. The plasma inhomogeneity changes the spatial distribution of the waves. The spatial distribution of the waves is fully determined by the distribution of plasma inhomogeneities. The possible applications to the theory of radio emission associated with electron beams are discussed.

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Propagation of a fast electron cloud in a solar-like plasma of decreasing density

Cited by 18 publications

References 22 publications

A review of solar type III radio bursts

A review of solar type III radio bursts

Plasma Emission by Nonlinear Electromagnetic Processes

Dynamics of electron beams in the solar corona plasma with density fluctuations

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