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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]
Chromosphere literally means “sphere of color” and is the second of the Sun’s three main layers. Temperatures in the chromosphere range from 6,700 degrees F near the surface and rise up to ...
The Sun's corona lies above the chromosphere and extends millions of kilometres into outer space. Coronal light is typically obscured by diffuse sky radiation and glare from the solar disk, but can be easily seen by the naked eye during a total solar eclipse or with a specialized coronagraph . [ 1 ]
The Sun's atmosphere is composed of five layers: the photosphere, the chromosphere, the transition region, the corona, and the heliosphere. The coolest layer of the Sun is a temperature minimum region extending to about 500 km above the photosphere, and has a temperature of about 4,100 K . [ 77 ]
The sun's chromosphere may be visible briefly; it would look like a thin, red layer around the sun. Red, tongue-like protrusions extending off the surface of the sun, called prominences, may also ...
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] They move upwards with speeds between 15 and 110 km/s from the photosphere and last a few minutes each [1] before falling back to the solar atmosphere. [2]
Indeed, along the very edge of the disappearing sun at the start and end of totality, an arc of ruby red or fuchsia associated with the solar chromosphere appeared. It looked bright red because ...
The solar transition region is a region of the Sun's atmosphere between the upper chromosphere and corona. [1] [2] It is important because it is the site of several unrelated but important transitions in the physics of the solar atmosphere: