The evolution of active regions (AR) from their emergence through their long decay process
is of fundamental importance in solar physics. Since large-scale flux is generated by the …

The question of what heats the solar corona remains one of the most important problems in
astrophysics. Finding a definitive solution involves a number of challenging steps, beginning …

X-ray emission from stars in the cool half of the Hertzsprung-Russell diagram is generally
attributed to the presence of a magnetic corona that contains plasma at temperatures …

The corona is a layer of hot plasma that surrounds the Sun, traces out its complex magnetic
field, and ultimately expands into interplanetary space as the supersonic solar wind …

We demonstrate that a three-dimensional magnetohydrodynamic (MHD) simulation of the
corona can model its global plasma density and temperature structure with sufficient …

Determining the heating mechanism (or mechanisms) that causes the outer atmosphere of
the Sun, and many other stars, to reach temperatures orders of magnitude higher than their …

We report new magnetic field measurements for 14 classical T Tauri stars (CTTSs). We
combine these data with one previous field determination in order to compare our observed …

We use soft X-ray and magnetic field observations of the Sun (quiet Sun, X-ray bright points,
active regions, and integrated solar disk) and active stars (dwarf and pre–main-sequence) to …

Magnetic fields are hypothesized to inflate the radii of low-mass stars—defined as less
massive than 0.8 M☉—in detached eclipsing binaries (DEBs). We investigate this …

This review focuses on the processes that energize and trigger M-and X-class solar flares
and associated flux-rope destabilizations. Numerical modeling of specific solar regions is …