Guillaume Aulanier

TL;DR: In this article, the authors focus on non-eruptive solar prominences, and describe recent progress in four areas of prominence research: (1) magnetic structure deduced from observations and models, (2) the dynamics of prominence plasmas (formation and flows), (3) magneto-hydrodynamic (MHD) waves in prominence and (4) the formation and large-scale patterns of the filament channels in which promine are located.

TL;DR: In this article, a zero-β magnetohydrodynamic (MHD) simulation of an initially potential, asymmetric bipolar field, which evolves by means of simultaneous slow magnetic field diffusion and sub-Alfvenic, line-tied shearing motions in the photosphere, is used to analyze the physical mechanisms that form a three-dimensional coronal flux rope and later cause its eruption.

TL;DR: In this article, the authors analyzed transition region and coronal Explorer and Solar and Heliospheric Observatory/Michelson Doppler Imager observations of a confined flare presenting a closed circular ribbon.

TL;DR: In this article, a nonlinear force-free field (NLFFF) model was applied to the highest resolution and quality vector-magnetographic data observed by the recently launched Hinode satellite on NOAA AR 10930 around the time of a powerful X3.4 flare.

TL;DR: In this article, it was shown that a global instability of the magnetic configuration is present when the current channel is located at a coronal height, h, large enough so that the decay index of the potential field, ∂ln |B p|/∂ln h, is larger than a critical value.