Electromagnetic heavy‐ion/proton instabilities

Wang, Joseph J.; Gary, S. Peter; Liewer, Paulett C.

doi:10.1029/1999ja900333

Cited by 5 publications

(7 citation statements)

References 15 publications

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“…Electromagnetic heavy-ion/proton instabilities driven by the relative velocity of two distinct ion components were generally studied by means of linear theory and non-linear numerical hybrid simulation by Wang et al (1999). Linear dispersion theory (see again the discussion in the previous Subsection 6.5) predicts that the fastest growing mode is the right hand polarised proton beam instability.…”

Section: Regulation Of the Ion Differential Motionmentioning

confidence: 99%

Kinetic Physics of the Solar Corona and Solar Wind

Marsch

2006

Living Rev. Solar Phys.

673

581

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Kinetic plasma physics of the solar corona and solar wind are reviewed with emphasis on the theoretical understanding of the in situ measurements of solar wind particles and waves, as well as on the remote-sensing observations of the solar corona made by means of ultraviolet spectroscopy and imaging. In order to explain coronal and interplanetary heating, the microphysics of the dissipation of various forms of mechanical, electric and magnetic energy at small scales (e.g., contained in plasma waves, turbulences or non-uniform flows) must be addressed. We therefore scrutinise the basic assumptions underlying the classical transport theory and the related collisional heating rates, and also describe alternatives associated with wave-particle interactions. We elucidate the kinetic aspects of heating the solar corona and interplanetary plasma through Landau-and cyclotron-resonant damping of plasma waves, and analyse in detail wave absorption and micro instabilities. Important aspects (virtues and limitations) of fluid models, either single-and multi-species or magnetohydrodynamic and multi-moment models, for coronal heating and solar wind acceleration are critically discussed. Also, kinetic model results which were recently obtained by numerically solving the Vlasov-Boltzmann equation in a coronal funnel and hole are presented. Promising areas and perspectives for future research are outlined finally.

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Section: Regulation Of the Ion Differential Motionmentioning

confidence: 99%

Kinetic Physics of the Solar Corona and Solar Wind

Marsch

2006

Living Rev. Solar Phys.

673

581

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“…Perhaps one of the őrst studies of xenon beam coupling with ambient proton plasma was conducted by Wang, who identiőed three mechanisms by which these interactions take place: particle/particle Coulomb collisions, as well as łprocesses [that] operate in collisionless plasmas and are sensitive functions of... the angle between the solar wind velocity and the interplanetary magnetic őeld" [22].…”

Section: B Prior Workmentioning

confidence: 99%

“…While these wave components are typically negligible, they may become more signiőcant when integrated over paths about the Earth. This model also neglects the free energy carried from the ion beam that may excite plasma instabiltieis, which may lead to scattering of beam ions through wave-particle interactions outside of the thruster exit on the order of kilometers [22].…”

Section: B Ion Trajectory Simulation Processesmentioning

confidence: 99%

Simulations of Xenon Beam Ions Emitted from Electric Thrusters in Earth's Magnetosphere

Sampson

Crofton

2022

Preprint

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This study sought to characterize the behavior of exhausted electric thruster xenon ions in the near-Earth magnetospheric environment as functions of various trajectory and particle attributes. This was done via simulation using the AeroTracer program, a software tool which computes ion trajectories within the magnetosphere by applying an adaptive step-size Runge-Kutta technique to the fully relativistic Lorentz equation. Over 3,800 independent simulations were performed, with variables including release position, release energy and direction, ion charge, and orbital phase. Initial release altitude was a major driver in determining whether the ion eventually fell to Earth (BMA), remained trapped by the simulation's end (MNS), or traveled beyond the magnetosphere (LTS). Ions expelled at the highest altitudes investigated -60,000 km and above -almost invariably were lost to space. Like altitude, increasing inclination and energy were important factors that reduced trapping, affecting the outcome probabilities. Higher charge state produced strong improvement of trapping capability. Effects of orbital phase, day of year and solar cycle phase were also apparent. A transition region was found in the 20,000 km to 60,000 km altitude range, within which the sensitivity of outcomes to parameter variation increased. The ordered sequence MNS > BMA > LTS was found to be consistent with decreasing confinement capability, and it was manifested consistently as parameters were varied.

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“…According to their differences in ion type, electromagnetic ion-ion instabilities can be roughly classified into electromagnetic alpha-proton [15,16], heavy-ion-proton [17], and electromagnetic proton-proton instabilities [18][19][20][21][22]. An investigation into the electromagnetic alpha-proton instability showed that during nonlinear evolution, the wavenumber, frequency, and propagation angle of the oblique Alfvén mode all drift to smaller values.…”

Section: Introductionmentioning

confidence: 99%

“…An investigation into the electromagnetic alpha-proton instability showed that during nonlinear evolution, the wavenumber, frequency, and propagation angle of the oblique Alfvén mode all drift to smaller values. A study of heavy-ionproton instability [17] revealed that the velocity threshold of the right-handed polarized ion-ion resonant instability decreases with a decrease in the gyrofrequency of the beam ions.…”

Section: Introductionmentioning

confidence: 99%

A simulation study of protons heated by left/right-handed Alfvén waves generated by electromagnetic proton–proton instability

Yao¹,

Zhao²,

Ye³

et al. 2021

Plasma Sci. Technol.

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Most protons in the solar wind belong to one of two different populations, the less dense beam protons and the denser core protons. The beam protons, with a velocity of (1-2) V A (V A is the local Alfvén speed), always drift relative to the core protons; this kind of distribution is unstable and stimulates several kinds of wave mode. In this study, using a 2D hybrid simulation model, we find that the original right-handed elliptically polarized Alfvén waves become linearly polarized, and eventually become right-handed and circularly polarized. Given that linearly polarized waves are a superposition of left-handed and right-handed waves, cyclotron resonance in the right-handed/left-handed component heats beam/core protons perpendicularly. The resonance between beam protons and right-handed polarized waves is stronger when the beam relative density is lower, resulting in more dramatic perpendicular heating of beam protons, whereas the situation is reversed when the beam relative density is larger.

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Electromagnetic heavy‐ion/proton instabilities

Cited by 5 publications

References 15 publications

Kinetic Physics of the Solar Corona and Solar Wind

Kinetic Physics of the Solar Corona and Solar Wind

Simulations of Xenon Beam Ions Emitted from Electric Thrusters in Earth's Magnetosphere

A simulation study of protons heated by left/right-handed Alfvén waves generated by electromagnetic proton–proton instability

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