Joe Giacalone

TL;DR: In this article, the authors present a new analysis of the transport of cosmic rays in a turbulent magnetic field that varies in all three spatial dimensions using a numerical simulation that integrates the trajectories of an ensemble of test particles from which they obtain diffusion coefficients based on the particle motions.

TL;DR: In this article, the authors consider the effect of preexisting, large-scale, broadband turbulent density fluctuations on propagating hydromagnetic shock waves and find that the density fluctuations not only distort the shape of the shock front and lead to a turbulent postshock fluid, but also produce a number of important changes in the post-shock magnetic field.

TL;DR: This paper provides a comprehensive review of the current state of knowledge of these important phenomena, and summarizes some of the key questions that will be addressed by two upcoming missions—NASA's Solar Probe Plus and ESA's Solar Orbiter.

TL;DR: The particles are used to study the mixing of the interplanetary magnetic field that is due to random walk and deduce an average timescale of 3.2 hr for these features, which corresponds to a length of approximately 0.03 AU.

TL;DR: In this paper, the authors consider the foundations of 1-and 2-dimensional shock simulations in which the physical quantities are independent of a coordinate which is not parallel to the magnetic field and show analytically that the ions are effectively tied to the convected magnetic lines of force because of the presence of an ignorable spatial coordinate.