Nonrelativistic electron stream propagation in the solar atmosphere and type III radio bursts

Magelssen, G. R.; Smith, D. F.

doi:10.1007/bf00150886

Cited by 126 publications

(68 citation statements)

References 33 publications

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“…Numerical work by e.g. Takakura & Shibahashi (1976); Magelssen & Smith (1977); Kontar et al (1998);Mel'nik et al (1999) confirmed that the beam-plasma structure could resolve the problem.…”

Section: Electron Beam Persistencementioning

confidence: 91%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

330

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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“…Numerical work by e.g. Takakura & Shibahashi (1976); Magelssen & Smith (1977); Kontar et al (1998);Mel'nik et al (1999) confirmed that the beam-plasma structure could resolve the problem.…”

Section: Electron Beam Persistencementioning

confidence: 91%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

330

217

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“…with ω pe = 2π f pe (Magelssen & Smith 1977). Here, the full reduced distribution function is composed of that of the accelerated electrons F acc and the Maxwellian one …”

Section: Intoduction To Shock Drift Accelerationmentioning

confidence: 99%

Electron beams generated by shock waves in the solar corona

Mann¹,

Klassen

2005

A&A

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Abstract. Beams of energetic electrons can be generated by shock waves in the solar corona. At the Sun shock waves are produced either by flares and/or by coronal mass ejections (CMEs). They can be observed as type II bursts in the solar radio radiation. Shock accelerated electron beams appear as rapidly drifting emission stripes (so-called "herringbones") in dynamic radio spectra of type II bursts. A large sample of type II bursts showing "herringbones" was statistically analysed with respect to their properties in dynamic radio spectra. The electron beams associated with the "herringbones" are considered to be generated by shock drift acceleration. Then, the accelerated electrons establish a shifted loss-cone distribution in the upstream region of the associated shock wave. Such a distribution causes plasma instabilities leading to the emission of radio waves observed as "herringbones". Consequences of a shifted loss-cone distribution of the shock accelerated electrons are discussed in comparison with the observations of "herringbones" within solar type II radio bursts.

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“…However, the mechanism of the merging process is unclear. One suggestion (Magelssen & Smith 1977) is that multiple beams are injected over a period of time, and that propagation causes them to lose their individual identities and form just one beam. A quantitative understanding of the mechanism of type III merging is important for tracing beam paths that lead to the IPM and interpreting acceleration processes.…”

Section: Introductionmentioning

confidence: 99%

“…Although beam and wave dynamics in a one-dimensional (1D) source region have been simulated (e.g., Magelssen & Smith 1977;Grognard 1985;Kontar & Pecseli 2002;Li et al 2006aLi et al , 2006b, the linked remote radiation has not been simulated so far. The first aim here is to develop a 3D model to study remote type III radiation, and present the first simulated dynamic spectra of a group of coronal type IIIs.…”

Section: Introductionmentioning

confidence: 99%

Simulated Dynamic Spectra: A Group of Coronal Type III Bursts

2007

ApJ

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First simulations are presented for the dynamic spectra of a group of coronal type III bursts that are observed remotely at Earth. A three-dimensional model is developed, including the structure of the source region, dynamics of electron beams, Langmuir, ion-sound, and electromagnetic waves within the source, and propagation of radiation to Earth. For realistic coronal and beam acceleration parameters, the simulation results are consistent with the general characteristics of type III bursts. We demonstrate that multiple radio bursts at high frequencies in the group merge at low frequencies, due mainly to a previously proposed mechanism which leads to merging of beams in the presence of beams and Langmuir waves only. The radio flux after the merging, however, depends jointly on beam-wave and wave-wave interactions and propagation effects.

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Nonrelativistic electron stream propagation in the solar atmosphere and type III radio bursts

Cited by 126 publications

References 33 publications

A review of solar type III radio bursts

A review of solar type III radio bursts

Electron beams generated by shock waves in the solar corona

Simulated Dynamic Spectra: A Group of Coronal Type III Bursts

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