The solar wind is a magnetized plasma and as such exhibits collective plasma behavior
associated with its characteristic spatial and temporal scales. The characteristic length …

Magnetohydrodynamic (MHD) activity, including waves and turbulence, has been a focus of
attention in solar wind research for several decades, owing to the wealth of available …

This book provides an overview of solar wind turbulence from both the theoretical and
observational perspective. It argues that the interplanetary medium offers the best …

In situ measurements of the solar wind have been available for almost 60 years, and in that
time plasma physics simulation capabilities have commenced and ground‐based solar …

A phenomenological theory describes radial evolution of plasma turbulence in the solar
wind from 1 to 50 astronomical units. The theory includes a simple closure for local …

The dissipation of turbulence in the weakly collisional solar wind plasma is governed by
unknown kinetic mechanisms. Two candidates have been suggested to play an important …

Structures in the solar wind result from two basic mechanisms: structures injected or
imposed directly by the Sun, and structures formed through processing en route as the solar …

A connection between kinetic processes and intermittent turbulence is observed in the solar
wind plasma using measurements from the Wind spacecraft at 1 AU In particular, kinetic …

Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy
to cascade to small scales where they are eventually dissipated, adding heat to the plasma …

Abstract Properties of the turbulent cascade from fluid to kinetic scales in collisionless
plasmas are investigated by means of large-size 3D hybrid (fluid electrons, kinetic protons) …