Asymmetric Electron Distributions in the Solar Wind

Rha, Kicheol; Ryu, Chang‐Mo; Yoon, Peter H.

doi:10.1088/2041-8205/775/1/l21

Cited by 26 publications

(3 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Ziebell et al, 2008a,b;Pavan et al, 2009a,b;Ziebell et al, 2011Ziebell et al, , 2012 such as heating of the background plasma (e.g. Yoon et al, 2012a;Rha et al, 2013). However the 1-d dynamics are generally expected to dominate.…”

Section: Quasi-linear Theorymentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

334

217

View full text Add to dashboard Cite

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.

show abstract

Section: Quasi-linear Theorymentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

334

217

View full text Add to dashboard Cite

show abstract

“…In general, it is expected that unless T T i e is small, ion-sound waves may heavily damp, thus prohibiting the three-wave resonant interaction. However, numerical solutions of the equations of the electrostatic weak turbulence theory as well as the electrostatic PIC simulation of the electron beam-plasma instability show that the three-wave interaction involving the S mode waves may still be operative even when T T i e is as high as an order of unity (Yoon et al 2012b;Rha et al 2013). We choose the value specified here only because we had adopted such a ratio in our previous studies such that we may directly compare the findings from the present investigation against the previous results (Ziebell et al 2001(Ziebell et al , 2008a(Ziebell et al , 2008b(Ziebell et al , 2011(Ziebell et al , 2012.…”

Section: Numerical Analysismentioning

confidence: 99%

Plasma Emission by Nonlinear Electromagnetic Processes

Ziebell

Yoon

Petruzzellis

et al. 2015

ApJ

View full text Add to dashboard Cite

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.

show abstract

“…Until now, the few attempts that have been made for a direct comparison, either qualitative or quantitative, between the results obtained from the weak turbulence theory and from numerical simulations have all been of a limited scope. Rha et al (2013) employed PIC simulation to test a theory for the generation of asymmetric superthermal tails in the electronic distribution function. According to the theory (Yoon et al 2012a), asymmetric tails can be created due to the nonlinear interactions of electrons with L and S waves, when the ion-electron temperature ratio (T i /T e ) varies within the range 0.1 T i /T e 1.…”

Section: Introductionmentioning

confidence: 99%

Particle-in-cell and Weak Turbulence Simulations of Plasma Emission

Lee

Ziebell

Yoon

et al. 2019

ApJ

View full text Add to dashboard Cite

The plasma emission process, which is the mechanism for solar type II and type III radio bursts phenomena, is studied by means of particle-in-cell and weak turbulence simulation methods. By plasma emission, it is meant as a loose description of a series of processes, starting from the solar flare associated electron beam exciting Langmuir and ion-acoustic turbulence, and subsequent partial conversion of beam energy into the radiation energy by nonlinear processes. Particle-in-cell (PIC) simulation is rigorous but the method is computationally intense, and it is difficult to diagnose the results. Numerical solution of equations of weak turbulence (WT) theory, termed WT simulation, on the other hand, is efficient and naturally lends itself to diagnostics since various terms in the equation can be turned on or off. Nevertheless, WT theory is based upon a number of assumptions. It is, therefore, desirable to compare the two methods, which is carried out for the first time in the present paper with numerical solutions of the complete set of equations of the WT theory and with two-dimensional electromagnetic PIC simulation. Upon making quantitative comparisons it is found that WT theory is largely valid, although some discrepancies are also found. The present study also indicates that it requires large computational resources in order to accurately simulate the radiation emission processes, especially for low electron beam speeds. Findings from the present paper thus imply that both methods may be useful for the study of solar radio emissions as they are complementary.

show abstract

Asymmetric Electron Distributions in the Solar Wind

Cited by 26 publications

References 37 publications

A review of solar type III radio bursts

A review of solar type III radio bursts

Plasma Emission by Nonlinear Electromagnetic Processes

Particle-in-cell and Weak Turbulence Simulations of Plasma Emission

Contact Info

Product

Resources

About