Coronal loops are the building blocks of the X-ray bright solar corona. They owe their
brightness to the dense confined plasma, and this review focuses on loops mostly as …

Coronal holes are the lowest density plasma components of the Sun's outer atmosphere,
and are associated with rapidly expanding magnetic fields and the acceleration of the high …

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

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 …

Recent observations of coronal loops in EUV wavelengths with the Transition Region and
Coronal Explorer (TRACE) and the Extreme-Ultraviolet Imaging Telescope (EIT) on the …

The heating of the solar corona has been a fundamental astrophysical issue for over sixty
years. Over the last decade in particular, space-based solar observatories (Yohkoh, SOHO …

The first observations of ultraviolet spectral line profiles and intensities from the extended
solar corona (ie, more than 1.5 solar radii from Sun-center) were obtained on 13 April 1979 …

We present a model of magnetohydrodynamic (MHD) turbulence in the extended solar
corona that contains the effects of collisionless dissipation and anisotropic particle heating …

Nanoflare models for heating the solar corona usually assume magnetic braiding and
reconnection as the source of the energy. However, recent observations at record spatial …

We explore some of the consequences of the magnetic carpet for coronal heating.
Observations show that most of the magnetic flux in the quiet Sun emerges as ephemeral …