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The red color of the chromosphere could be seen during the solar eclipse of August 11, 1999.. The density of the Sun's chromosphere decreases exponentially with distance from the center of the Sun by a factor of roughly 10 million, from about 2 × 10 −4 kg/m 3 at the chromosphere's inner boundary to under 1.6 × 10 −11 kg/m 3 at the outer boundary. [7]
For example, jetting phenomena observed in coronal and chromospheric temperatures are sometimes referred to as coronal jets and chromospheric jets (or chromospheric surges), respectively, and when observed in X-rays, extreme ultraviolet, white light, and Hα are sometimes referred to as X-ray jets, EUV jets, white-light jets, and Hα jets (or ...
Chromospheric Helium-I Imaging Photometer (CHIP) observes at a wavelength which is an emission line for non-ionized helium (He I) in order to monitor the chromosphere. [3] The Polarimeter for Inner Coronal Studies (PICS) produced H-alpha disk and limb digital images from 1994 to 1997. It was replaced by the CS60. [3]
chromospheric activity index A parameter indicating the magnetic activity in a star's chromosphere. One measure of this activity is log R′ HK, where R′ HK is the ratio of the equivalent width of a star's singly ionized calcium H and K lines, after correction for photospheric light, to the bolometric flux. [4]
Spicules near the solar limb. They appear as dark "hairs" above the solar surface. In solar physics, a spicule, also known as a fibril or mottle, [a] is a dynamic jet of plasma in the Sun's chromosphere about 300 km in diameter. [1]
Classically, plage have been defined as regions that are bright in Hα and other chromospheric emission lines. With modern imaging, most researchers now identify plage based on the photospheric magnetic field concentration of the faculae below. The magnetic field of plage is confined to the intergranular lanes in the photosphere with a strength ...
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The CHROMospheric Imaging Spectrometer [10] (CHROMIS) was installed in 2016. It is similar to CRISP (but so far without polarimetry) and designed for use at wavelengths in the range 380–500 nm. In particular, CHROMIS is optimized for use in the Ca II H and K lines, which are formed in the upper chromosphere.