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 …

X-ray and ultraviolet (UV) observations of the outer solar atmosphere have been used for
many decades to measure the fundamental parameters of the solar plasma. This review …

Energy is required to heat the outer solar atmosphere to millions of degrees (refs,) and to
accelerate the solar wind to hundreds of kilometres per second (refs). Alfvén waves …

The Sun's outer atmosphere, or corona, is heated to millions of degrees, considerably hotter
than its surface or photosphere. Explanations for this enigma typically invoke the deposition …

Observational and theoretical evidence suggests that coronal heating is impulsive and
occurs on very small cross-field spatial scales. A single coronal loop could contain a …

The Sun's corona is millions of degrees hotter than its 5000 K photosphere. This heating
enigma is typically addressed by invoking the deposition at coronal heights of nonthermal …

Strongly damped Doppler shift oscillations are observed frequently associated with flarelike
events in hot coronal loops. In this paper, a review of the observed properties and the …

The solar active region 10938 has been observed from the disk center to the west limb with
the Hinode EUV Imaging Spectrometer. In the disk-center observation, subsonic upflow …

ABSTRACT A well-known behavior of EUV light curves of discrete coronal loops is that the
peak intensities of cooler channels or spectral lines are reached at progressively later times …

From Doppler velocity maps of active regions constructed from spectra obtained by the EUV
Imaging Spectrometer (EIS) on the Hinode spacecraft we observe large areas of outflow (20 …