In adiabatically stratified cluster gas the MTI saturates via large plumes destroyed by shear, producing turbulent kinetic energy that scales as χ ω_T.
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8 Pith papers cite this work, alongside 184 external citations. Polarity classification is still indexing.
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2026 8representative citing papers
First kinetic PIC simulation of expanding turbulent solar wind shows preferential parallel electron energization forming power-law tails under weakly compressive Alfvénic conditions.
Energy-dependent polarization angle variability distinguishes reconnection from turbulence as the driver of blazar flares, with Mrk 421 and 1ES 1959+650 data favoring reconnection.
In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
In multispecies relativistic turbulence, energization occurs at reconnection current sheets driven by the divergence of the relativistic pressure tensor, with electrons accelerated more efficiently than positrons due to species imbalance.
Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
Curvature acceleration in strong Alfvénic turbulence saturates due to diminishing energy exchange efficiency, producing particle distributions f(p) ∝ p^{-3} (non-relativistic) and f(γ) ∝ γ^{-3} (ultrarelativistic).
Entity PIC code updated with up to 11th-order current deposit and generalized field stencils, with tests showing improved conservation properties and suppression of numerical effects.
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Formation of Suprathermal Electron Populations in the Expanding, Turbulent Solar Wind
First kinetic PIC simulation of expanding turbulent solar wind shows preferential parallel electron energization forming power-law tails under weakly compressive Alfvénic conditions.