During solar flares a tremendous amount of magnetic energy is released and transported
through the Sun's atmosphere and out into the heliosphere. Despite over a century of study …

Magnetic storms on stars manifest as remarkable, randomly occurring changes of the
luminosity over durations that are tiny in comparison to the normal evolution of stars. These …

Solar flares are transient yet dramatic events in the atmosphere of the Sun, during which a
vast amount of magnetic energy is liberated. This energy is subsequently transported …

M dwarf flares observed by the Transiting Exoplanet Survey Satellite (TESS) sometimes
exhibit a peak-bump light-curve morphology, characterized by a secondary, gradual peak …

Solar flares are 3D phenomena, but modeling a flare in 3D, including many of the important
processes in the chromosphere, is a computational challenge. Accurately modeling the …

Using observations from the Solar Dynamics Observatory's Atmosphere Imaging Assembly
and the Ramaty High Energy Solar Spectroscopic Imager, we present novel measurements …

Coronal flare emission is commonly observed to decay on timescales longer than those
predicted by impulsively driven, one-dimensional flare loop models. This discrepancy is …

Theoretically, coronal mass ejection (CME) kinematics are related to magnetic reconnection
processes in the solar corona. However, the current quantitative understanding of this …

Solar flares are observed and classified according to their intensity measured with the
Geostationary Operational Environmental Satellite (GOES) X-ray Sensors. We show that the …

Coronal rain is ubiquitous in flare loops, forming shortly after the onset of the solar flare.
Rain is thought to be caused by a thermal instability, a localized runaway cooling of material …