Proton-Alpha Drift Instability of Electromagnetic Ion-Cyclotron Modes: Quasilinear Development

Shaaban, S. M.; Lazar, M.; Yoon, Peter H.; Poedts, Stefaan; Lopez, Rigoberto

doi:10.3390/physics3040075

Cited by 2 publications

(3 citation statements)

References 34 publications

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“…While there is some qualitative agreement in the evolution of the temperature anisotropies and drift velocity in Case 1 with the quasi-linear results of Shaaban et al (2021) in their Case 4, the model parameters are substantially different for direct comparison.…”

Section: Temporal Evolution Of Anisotropies Energies and Drift Speedmentioning

confidence: 73%

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Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia

Ofman,

Boardsen,

Jian

et al. 2023

ApJ

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Past observations show that solar wind (SW) acceleration occurs inside the sub-Alfvénic region, reaching the local Alfvén speed at typical distances ∼10–20 solar radii (R s ). Recently, Parker Solar Probe (PSP) traversed regions of sub-Alfvénic SW near perihelia in encounters E8–E12 for the first time, providing data in these regions. It became evident that the properties of the magnetically dominated SW are considerably different from the super-Alfvénic wind. For example, there are changes in the relative abundances and drift of α particles with respect to protons, as well as in the magnitude of magnetic fluctuations. We use data of the magnetic field from the FIELDS instrument, and construct ion velocity distribution functions (VDFs) from the sub-Alfvénic regions using Solar Probe ANalyzer for Ions data, and run 2.5D and 3D hybrid models of proton-α sub-Alfvénic SW plasma. We investigate the nonlinear evolution of the ion kinetic instabilities in several case studies, and quantify the transfer of energy between the protons, α particles, and the kinetic waves. The models provide the 3D ion VDFs at the various stages of the instability evolution in the SW frame. By combining observational analysis with the modeling results, we gain insights on the evolution of the ion instabilities, the heating and the acceleration processes of the sub-Alfvénic SW plasma, and quantify the exchange of energy between the magnetic and kinetic components. The modeling results suggest that the ion kinetic instabilities are produced locally in the SW, resulting in anisotropic heating of the ions, as observed by PSP.

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Section: Temporal Evolution Of Anisotropies Energies and Drift Speedmentioning

confidence: 73%

“…approach to study the evolution of proton-α anisotropic plasma was developed using macroscopic quasi-linear theory (e.g., Yoon et al 2015), demonstrating qualitative agreement with PIC models. Recently quasi-linear theory was applied to study the proton-α drift instability for a range of typical SW parameters (Shaaban et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia

Ofman,

Boardsen,

Jian

et al. 2023

ApJ

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“…As noted, the advantage of adopting the expanding-box paradigm is that one may work with the local wave kinetic equation, which is essentially the same as that of a uniform plasma theory (Seough & Yoon 2012;Moya & Navarro 2021;Navarro & Moya 2023). This implies that in other more complex situations, e.g., the solar-wind modeling with multiple ion (or electron) species, or charged particle species that contain relative drifts (Yoon et al 2015;Sarfraz et al 2016;Sarfraz 2018;Sarfraz & Yoon 2020;Shaaban et al 2021), we may formulate the basic equations either on the basis of expanding paradigm, or on the basis of steady-state macroscopic approach, but as far as the wave kinetic equation is concerned, one may choose to work in the framework of the local theory, which offers the advantage of mathematical simplicity.…”

Section: Adding Quasilinear Wave-particle Relaxation To the Expanding...mentioning

confidence: 99%

Expanding-box Quasilinear Model of the Solar Wind

Seough

Yoon

Nariyuki

et al. 2023

ApJ

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The expanding-box model of the solar wind has been adopted in the literature within the context of magnetohydrodynamics, hybrid, and full particle-in-cell simulations to investigate the dynamic evolution of the solar wind. The present paper extends such a method to the framework of self-consistent quasilinear kinetic theory. It is shown that the expanding-box quasilinear methodology is largely equivalent to the inhomogeneous steady-state quasilinear model discussed earlier in the literature, but a distinction regarding the description of wave dynamics between the two approaches is also found. The expanding-box quasilinear formalism is further extended to include the effects of a spiraling solar-wind magnetic field as well as collisional age effects. The present finding shows that the expanding-box quasilinear approach and the steady-state global-kinetic models may be employed interchangeably in order to address other more complex problems associated with the solar-wind dynamics.

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Proton-Alpha Drift Instability of Electromagnetic Ion-Cyclotron Modes: Quasilinear Development

Cited by 2 publications

References 34 publications

Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia

Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia

Expanding-box Quasilinear Model of the Solar Wind

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