William H. Matthaeus

TL;DR: In this article, the authors examine energetic charged particle diffusion perpendicular to a mean magnetic field B0 due to turbulent fluctuations in a plasma, relaxing the common assumption of axisymmetry around B0 and varying the ratio of two fluctuation components, a slab component with parallel wavenumbers and a two-dimensional (2D) component with perpendicular wenumbers.

TL;DR: In this article, the authors employ several measures to quantify the extent of Alfvenicity, such as the Alfven ratio, the normalized cross helicity, and the cosine of angle between velocity and magnetic fluctuations, and show that despite the overall impression that the solar wind sampled by Parker Solar Probe (PSP) during the first encounter is mostly highly Alfvenic.

TL;DR: In the context of space and astrophysical plasma turbulence and particle heating, several vocabularies emerge for estimating turbulent energy dissipation rate, including Kolmogorov-Yaglom third-order law and, in its various forms, the electromagnetic field on particles.

TL;DR: In this paper, the effect of driving frequency on the efficiency of turbulence generation through magnetic forcing is studied using kinetic hybrid simulations with fully kinetic ions and fluid electrons, and the efficiency is quantified by examining the energy input into magnetic field as well as the thermal energy for various driving frequencies.

TL;DR: In this paper, a simple analytic formula is used in conjunction with the simulation results to predict the maximum energy achievable in a particular plasma environment with the result that in solar flares reconnection is capable of accelerating particles to several GeV.