Scott H. Hawley

TL;DR: In this article, the authors tracked the birth and outflow of 50-100 of the most prominent moving coronal features and found that they originate about 3-4 R☉ from Sun center as radially elongated structures above the cusps of helmet streamers.

TL;DR: This work presents results of 3D numerical simulations using a finite difference code featuring fixed mesh refinement (FMR), in which a subset of the computational domain is refined in space and time.

TL;DR: The magnetic field strengths and field-line divergence rates in coronal holes can be related empirically to the bulk speed and the mass and energy flux densities of the solar wind plasma as discussed by the authors.

TL;DR: In this paper, the authors presented a study of black hole threshold phenomena for a self-gravitating, massive complex scalar field in spherical symmetry, where the massless field is used to perturb the boson star via a purely gravitational interaction, which results in a significant transfer of energy from the mass-less field to the massive field, and the resulting (unstable) critical solutions persist for a finite time before either dispersing most of the mass to infinity (leaving a diffuse remnant) or forming a black hole.

TL;DR: In this article, a suite of standardized testbeds for comparing approaches to the numerical evolution of Einstein's equations that are designed to both probe their strengths and weaknesses and to separate out different effects, and their causes, seen in the results are presented.