Two-dimensional time evolution of beam-plasma instability in the presence of binary collisions

Tigik, Sabrina F.; Ziebell, L. F.; Yoon, Peter H.; Kontar, Eduard P.

doi:10.1051/0004-6361/201527271

Cited by 39 publications

(14 citation statements)

References 59 publications

(72 reference statements)

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“…2016; Tigik et al. 2016), where collisions are usually introduced by means of a collisional operator at the right-hand side of the Vlasov equation. The choice of the proper collisional operator remains an open problem.…”

Section: Solar Wind Heating: a Huge Problemmentioning

confidence: 99%

Solar wind collisional heating

Pezzi

2017

J. Plasma Phys.

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To properly describe heating in weakly collisional turbulent plasmas such as the solar wind, interparticle collisions should be taken into account. Collisions can convert ordered energy into heat by means of irreversible relaxation towards the thermal equilibrium. Recently, Pezzi et al. (Phys. Rev. Lett., vol. 116, 2016a, 145001) showed that the plasma collisionality is enhanced by the presence of fine structures in velocity space. Here, the analysis is extended by directly comparing the effects of the fully nonlinear Landau operator and a linearized Landau operator. By focusing on the relaxation towards the equilibrium of an out of equilibrium distribution function in a homogeneous force-free plasma, here it is pointed out that it is significant to retain nonlinearities in the collisional operator to quantify the importance of collisional effects. Although the presence of several characteristic times associated with the dissipation of different phase space structures is recovered in both the cases of the nonlinear and the linearized operators, the influence of these times is different in the two cases. In the linearized operator case, the recovered characteristic times are systematically larger than in the fully nonlinear operator case, this suggesting that fine velocity structures are dissipated more slowly if nonlinearities are neglected in the collisional operator.

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Section: Solar Wind Heating: a Huge Problemmentioning

confidence: 99%

Solar wind collisional heating

Pezzi

2017

J. Plasma Phys.

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“…Understanding these evolutions requires advanced theories and multi-scale modeling to combine exospheric mechanisms involving suprathermal electrons (e.g., velocity filtration), and effects of solar wind expansion (e.g., magnetic focusing and increase of parallel temperature) with diffusion in pitch angle and energy induced by collisions (at low distances in the outer corona) and by wave-particle interactions (Zouganelis et al 2005;Tigik et al 2016;Innocenti et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Characteristics of solar wind suprathermal halo electrons

Lazar

Pierrard

Poedts

et al. 2020

A&A

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A suprathermal halo population of electrons is ubiquitous in space plasmas, as evidence of their departure from thermal equilibrium even in the absence of anisotropies. The origin, properties, and implications of this population, however, are poorly known. We provide a comprehensive description of solar wind halo electrons in the ecliptic, contrasting their evolutions with heliospheric distance in the slow and fast wind streams. At relatively low distances less than 1 AU, the halo parameters show an anticorrelation with the solar wind speed, but this contrast decreases with increasing distance and may switch to a positive correlation beyond 1 AU. A less monotonic evolution is characteristic of the high-speed winds, in which halo electrons and their properties (e.g., number densities, temperature, plasma beta) exhibit a progressive enhancement already distinguishable at about 0.5 AU. At this point, magnetic focusing of electron strahls becomes weaker and may be counterbalanced by the interactions of electrons with wave fluctuations. This evolution of halo electrons between 0.5 AU and 3.0 AU in the fast winds complements previous results well, indicating a substantial reduction of the strahl and suggesting that significant fractions of strahl electrons and energy may be redistributed to the halo population. On the other hand, properties of halo electrons at low distances in the outer corona suggest a subcoronal origin and a direct implication in the overheating of coronal plasma via velocity filtration.

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“…Whilst this simplifies the models and is grounded by observations of electrons with small pitch angles at 1 AU, it is still a major simplification. Recent efforts have been undertaken (Ziebell et al, 2014(Ziebell et al, , 2015(Ziebell et al, , 2016Tigik et al, 2016) to model the plasma emission process in two velocity dimensions for a single point in space, taking into account all the steps involved in the plasma emission process. In the simulations by Ziebell et al (2015), fundamental emission was generated by Langmuir waves both with ionsound waves and by scattering.…”

Section: Electron Beam Propagationmentioning

confidence: 99%

“…These processes dominated initially, whilst over time the harmonic emission overtook the fundamental. Taking into account collisions, Tigik et al (2016) found that a wider plateau was formed in the distribution function and increased the tendency to isotropization.…”

Section: Electron Beam Propagationmentioning

confidence: 99%

A Review of Recent Solar Type III Imaging Spectroscopy

Reid

2020

Front. Astron. Space Sci.

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Two-dimensional time evolution of beam-plasma instability in the presence of binary collisions

Cited by 39 publications

References 59 publications

Solar wind collisional heating

Solar wind collisional heating

Characteristics of solar wind suprathermal halo electrons

A Review of Recent Solar Type III Imaging Spectroscopy

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