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 …

This paper reviews three important effects on energetic particles of corotating interaction
regions (CIRs) in the solar wind that are formed at the leading edges of high-speed solar …

Coronal holes are areas on the Sun with open magnetic field lines. They are a source region
of the solar wind, but how the wind emerges from coronal holes is not known. We observed …

The enlarged new edition of this textbook provides a comprehensive introduction to the
basic processes in plasmas and demonstrates that the same fundamental concepts describe …

An unsolved problem in plasma turbulence is how energy is dissipated at small scales.
Particle collisions are too infrequent in hot plasmas to provide the necessary dissipation …

Observations of solar wind from both large polar coronal holes (PCHs) during Ulysses' third
orbit showed that the fast solar wind was slightly slower, significantly less dense, cooler, and …

We present a quantitative estimate of the anisotropic power and scaling of magnetic field
fluctuations in inertial range magnetohydrodynamic turbulence, using a novel wavelet …

Ulysses is now completing its second solar polar orbit, dropping back down in latitude as the
Sun passes through its post‐maximum phase of the solar cycle. A mid‐sized circumpolar …

Models for the origin of the slow solar wind must account for two seemingly contradictory
observations: the slow wind has the composition of the closed-field corona, implying that it …

Observations by the RHESSI satellite of the large polarization of the prompt γ-ray emission
from γ-ray burst (GRB) 021206 imply that the magnetic field coherence scale is larger than …