Erratum: “Magnetic Pumping as a Source of Particle Heating and Power-law Distributions in the Solar Wind” (2017, ApJL, 850, L28)

Lichko, Emily; Egedal, J.; Daughton, W.; Kasper, J. C.

doi:10.3847/2041-8213/aaaaab

Cited by 1 publication

(8 citation statements)

References 1 publication

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“…This mechanism allows the plasma to effectively retain energy coming from large-scale turbulent fluctuations after a complete pump cycle. One of the outcomes of our work is that, as predicted by Lichko et al (2017), shorter cycles lead to greater energy retention, even when the scattering process is modeled self-consistently.…”

Section: Introductionmentioning

confidence: 79%

“…, where ò = 1, and solve Equation (14) to first order in ò. Whereas for ν = 0, ΔP and  B B are out of phase by π/2 and yield no net heating when integrated over one magnetic cycle period, collisions introduce a phase shift in ΔP which is maximized for ω = ν/3, irreversibly heating the plasma (see Lichko et al 2017, where ν is treated as a free parameter). A more general model of this effect is presented in Section 6.…”

Section: Theoretical Basismentioning

confidence: 99%

“…These authors estimated ΔP by assuming it is pinned to marginal stability with respect to the mirror and firehose microinstabilities. In a similar approach, and with application to the solar wind, Lichko et al (2017) considered heating and nonthermal particle energization under the assumption of a periodically compressing flux tube with a prescribed scattering frequency, in a process termed magnetic pumping.…”

Section: Introductionmentioning

confidence: 99%

“…Kulsrud (1983) refers to it as "frictional heating by nonuniform velocities," and Hollweg (1985) as "volumetric viscous heating rate." We will follow Lichko et al (2017) and refer to this mechanism as heating by magnetic pumping from now on. Magnetic pumping has the important property that it directly taps the energy of large-scale turbulence in weakly collisional plasmas.…”

Section: Introductionmentioning

confidence: 99%

“…In this work, we combine the approaches of Kunz et al (2011) and Lichko et al (2017) and present a heating mechanism acting via magnetic pumping in a periodically shearing, high-β plasma suitable for studying ICM conditions. The isotropizing effect necessary for the operation of magnetic pumping will be given by the scattering that mirror and firehose instabilities provide as they interact with the particles, and this will be self-consistently captured using 2.5 dimensional (i.e., electromagnetic fields and particles' momenta have three components but only vary in two spatial dimensions), fully kinetic particle-in-cell (PIC) simulations.…”

Section: Introductionmentioning

confidence: 99%

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A Heating Mechanism via Magnetic Pumping in the Intracluster Medium

Ley

Zweibel

Riquelme

et al. 2023

ApJ

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Turbulence driven by active galactic nuclei activity, cluster mergers, and galaxy motion constitutes an attractive energy source for heating the intracluster medium (ICM). How this energy dissipates into the ICM plasma remains unclear, given its low collisionality and high magnetization (precluding viscous heating by Coulomb processes). Kunz et al. proposed a viable heating mechanism based on the anisotropy of the plasma pressure under ICM conditions. The present paper builds upon that work and shows that particles can be heated by large-scale turbulent fluctuations via magnetic pumping. We study how the anisotropy evolves under a range of forcing frequencies, what waves and instabilities are generated, and demonstrate that the particle distribution function acquires a high-energy tail. For this, we perform particle-in-cell simulations where we periodically vary the mean magnetic field B (t). When B (t) grows (dwindles), a pressure anisotropy P ⊥ > P ∥(P ⊥ < P ∥) builds up (P ⊥ and P ∥ are, respectively, the pressures perpendicular and parallel to B (t)). These pressure anisotropies excite mirror (P ⊥ > P ∥) and oblique firehose (P ∥ > P ⊥) instabilities, which trap and scatter the particles, limiting the anisotropy, and providing a channel to heat the plasma. The efficiency of this mechanism depends on the frequency of the large-scale turbulent fluctuations and the efficiency of the scattering the instabilities provide in their nonlinear stage. We provide a simplified analytical heating model that captures the phenomenology involved. Our results show that this process can be relevant in dissipating and distributing turbulent energy at kinetic scales in the ICM.

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Section: Introductionmentioning

confidence: 79%

Section: Theoretical Basismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%