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 …

When discussing research in physics and in science more generally, it is common to ascribe
equal importance to the three components of the scientific trinity: theoretical, experimental …

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 …

In this review we will focus on a topic of fundamental importance for both astrophysics and
plasma physics, namely the occurrence of large-amplitude low-frequency fluctuations of the …

A comprehensive overview is presented of recent observational and theoretical results on
solar wind structures and fluctuations and magnetohydrodynamic waves and turbulence …

The fast solar wind's high speeds and non-thermal features require that considerable
heating occurs well above the Sun's surface. Two leading theories seem incompatible: low …

This paper presents a theoretical framework for understanding plasma turbulence in
astrophysical plasmas. It is motivated by observations of electromagnetic and density …

The magnetic field experiment on ACE provides continuous measurements of the local
magnetic field in the interplanetary medium. These measurements are essential in the …

Solar wind fluctuations are commonly regarded as a superposition of MHD waves, primarily
in the Alfvén mode. These MHD fluctuations are frequently assumed to possess “slab” or …

The dissipation range for interplanetary magnetic field fluctuations is formed by those
fluctuations with spatial scales comparable to the gyroradius or ion inertial length of a …