A corona is a type of plasma "atmosphere" of the Sun or other celestial body, extending millions of kilometers into space, most easily seen during a total solar eclipse, but also observable in a coronagraph. The Latin root of the word corona means crown.
The high temperature of the corona gives it unusual spectral features, which led some to suggest, in the 19th century, that it contained a previously unknown element, "coronium". These spectral features have since been traced to highly ionized iron (Fe-XIV) which indicates a plasma temperature in excess of 106 kelvin. The fact that the Sun has a million degree corona was first discovered by Gotrian in 1939 and Bengt Edlén in 1941 by identifying the coronal lines (observed since 1869) as
transitions from low lying metastable levels of the ground configuration
of highly ionized metals (the green FeXIV line at 5303 Å, but also the
red line FeX at 6374 Å).
Light from the corona comes from three primary sources, which are
called by different names although all of them share the same volume of
space. The K-corona (K for kontinuierlich, "continuous" in German) is created by sunlight scattering off free electrons; Doppler broadening of the reflected photospheric absorption lines completely obscures
them, giving the spectral appearance of a continuum with no absorption
lines. The F-corona (F for Fraunhofer)
is created by sunlight bouncing off dust particles, and is observable
because its light contains the Fraunhofer absorption lines that are seen
in raw sunlight; the F-corona extends to very high elongation angles from the Sun, where it is called the Zodiacal light.
The E-corona (E for emission) is due to spectral emission lines
produced by ions that are present in the coronal plasma; it may be
observed in broad or forbidden or hot spectral emission lines and is the main source of information about the corona's composition.