Asymmetric Solar Wind Electron Distributions

Yoon, Peter H.; Hong, J.; Kim, S.; Lee, Junggi; Lee, Junhyun; Park, Jongsun; Park, Kyungsun; Seough, Jungjoon

doi:10.1088/0004-637x/755/2/112

Cited by 35 publications

(26 citation statements)

References 30 publications

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“…This is why damping rates can be added in the Fourier transforms of the above Equations (1)-(3) derived from the systemʼs Hamiltonian (see, e.g., Krafft et al 2015a). Note finally that for homogeneous plasmas, the model and the approach used here lead to results qualitatively similar to those obtained on the basis of weak turbulence kinetic equations (e.g., Yoon et al 2012).…”

Section: Theoretical Backgroundmentioning

confidence: 52%

“…Their resonant decay through the channel     ¢ + ¢ produces backscattered Langmuir waves ¢ and ion sound waves ¢; if the daughter waves ¢ carry enough energy, they can encounter a second decay cascade (SDC) according to    ¢   + , as well as further cascades, until these processes become prohibited by kinematic effects. Such multiple decay processes have been considered by solving the weak turbulence kinetic equations (e.g., Yoon et al 2012) or the Zakharov equations (Krafft et al 2015a). In a onedimensional(1D)description, which is valid for the physical problem considered here as most of Langmuir waves in the solar wind are believed to be longitudinally polarized (Ergun et al 2008), the Langmuir waves ¢ and  coming from the first and the second cascades propagate, respectively, in the inverse and the same directions as the parent wave , i.e., as the electron beam.…”

Section: Introductionmentioning

confidence: 99%

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Electron Acceleration by Langmuir Waves Produced by a Decay Cascade

Krafft

Volokitin

2016

ApJ

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It was recently reported that a significant part of the Langmuir waveforms observed by the STEREO satellite during type III solar radio bursts are likely consistent with the occurrence of electrostatic decay instabilities, when a Langmuir wave  resonantly interacts with another Langmuir wave ¢ and an ion sound wave ¢ through the decay channel     ¢ + ¢. Usually such wave-wave interactions occur in regions of the solar wind where the presence of electronbeams can drive Langmuir turbulence tolevels allowing waves  to decay. Moreover, such solar wind plasmas can present long-wavelength, randomly fluctuating density inhomogeneities or monotonic density gradients which can significantlymodifythe development of such resonant instabilities. If some conditions are met, the waves can encounter a second decay cascade (SDC) according to    ¢   + . Analytical estimates and observations based on numerical simulations show that the Langmuir waves  produced by this SDC can accelerate beam particles up to velocities and kinetic energies exceedingtwo times the beam drift velocity v b and half the initial beam energy, respectively. Moreover, this process can be particularly efficient if thescattering effects of waves on the background plasma inhomogeneities have already accelerated a sufficient amount of beam electrons up to the velocity range where the phase velocities of the  waves are lying. The paper shows that the conditions necessary for such process to occur can be easily met in solar wind plasmas if the beam velocities do not exceed around 35 times the plasma thermal velocity.

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Section: Theoretical Backgroundmentioning

confidence: 52%

Section: Introductionmentioning

confidence: 99%

Electron Acceleration by Langmuir Waves Produced by a Decay Cascade

Krafft

Volokitin

2016

ApJ

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“…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

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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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“…In a recent work, Yoon et al (2012) relaxed this assumption by resorting back to the situation where the Langmuir turbulence is generated by the customary single electron beam, or bumpin-tail instability. Note that such a problem has already been investigated by Yoon et al (2005aYoon et al ( , 2005bYoon et al ( , 2006 and Rhee et al (2006).…”

Section: Introductionmentioning

confidence: 99%

“…Note that such a problem has already been investigated by Yoon et al (2005aYoon et al ( , 2005bYoon et al ( , 2006 and Rhee et al (2006). The key difference, however, is that unlike the previous works where the ion-to-electron temperature ratio was fixed, Yoon et al (2012) systematically varied T i /T e . In plasma physics it is well known that the ion-sound mode is heavily damped when T i /T e is high.…”

Section: Introductionmentioning

confidence: 99%

Asymmetric Electron Distributions in the Solar Wind

Rha

Ryu

Yoon

2013

ApJ

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A plausible mechanism responsible for producing asymmetric electron velocity distribution functions in the solar wind is investigated by means of one-dimensional electrostatic particle-in-cell (PIC) simulation. A recent paper suggests that the variation in the ion-to-electron temperature ratio influences the nonlinear wave-particle dynamics such that it results in the formation of asymmetric distributions. The present PIC code simulation largely confirms this finding, but quantitative differences between the weak turbulence formalism and the present PIC simulation are also found, suggesting the limitation of the analytical method. The inter-relationship between the asymmetric electron distribution and the ion-to-electron temperature ratio may be a new useful concept for the observation.

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Asymmetric Solar Wind Electron Distributions

Cited by 35 publications

References 30 publications

Electron Acceleration by Langmuir Waves Produced by a Decay Cascade

Electron Acceleration by Langmuir Waves Produced by a Decay Cascade

A review of solar type III radio bursts

Asymmetric Electron Distributions in the Solar Wind

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