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A background color image was created from an HDR Pro stack in Photoshop CC 2017. Exposure sets were then averaged together in Images Plus. Exposures longer than 1/15th second were dark subtracted with 64 matching dark exposures. Processing the CoronaĮach individual image of the corona at various shutter speeds were calibrated with 64 flats, 64 bias in Images Plus. Image Acquisition was completely automated with Solar Eclipse Maestro. Only the Earthshine, which was recorded in the longest exposures, was very difficult to see visually. The human eye, a remarkable visual instrument, can encompass almost the entire brightness range of the total eclipse. They are then composited together with special high-dynamic range techniques which more closely approximate what the human eye can see.
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To deal with this huge dynamic range, a series of different exposures are made during totality, each correctly recording just one part of the corona. The long 2 second exposures will completely overexpose the bright portions of the scene, and short 1/4000th second exposures will not record any of the faint outer corona.
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The correct exposure for the bright red prominences along the Sun's limb is 1/4000th second at f/6.3 at ISO 200.
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The correct exposure for the sky background and outer corona is 2 seconds at f/6.3 at ISO 200. Normal cameras can not record this much of a difference in brightness in a single exposure. The Sun's corona has a tremendous brightness range spanning more than 14 photographic stops.
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The IRF (Infrared fluorescence) Corona is caused by infrared fluorescence of silicon nanoparticles produced by interaction of the K- and F-corona and sunlight.
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The Fl (fluorescence) Corona is caused by resonance fluorescence of molecules and free radicals produced by interactions of the K- and F-corona, solar wind and sunlight. The S (Sublimation) Corona is made up of the emission of low ionized atoms produced by sublimation of dust particles in relatively cold parts of the corona. The T (Thermal) Corona is caused by thermal emission in the infrared region by interplanetary dust. Scientists list several other types of coronas which are generally only visible in the infrared: The E-corona is much fainter than the K and F coronas. The E (Emission) Corona is made up of narrow spectral emission lines produced by ions in the hot plasma. The F corona is the brightest part of the corona beyond 1.5 solar radii from the Sun's limb. The F (Fraunhofer) Corona is comprised of sunlight scatter by, or reflected off, dust particles and actually merges into the Zodiacal light. The K-corona is the brightest part of the visible corona out to 1.5 solar radii. The Fraunhofer lines of the photospheric spectrum are smeared out so that the spectrum of the K corona is almost a pure continuum. The K (Kontinuierlich) Corona is closest to the limb of the Sun and is made up of sunlight scattered by free electrons. The light from the visible corona comes from three sources: The corona extends millions of miles into space and is made up of super-heated plasma at about 2 million degrees K.
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It is one of the rarest and most beautiful sights in nature and seeing it may be a once-in-lifetime experience. The solar corona can only be seen during a total eclipse of the Sun. The corona is very thin, but has a temperature of more than a million degrees Kelvin and actually gets hotter farther away from the Sun. Intricate detail in the corona is caused by the Sun's magnetic fields which get twisted up and when they release a tremendous amount of stored magnetic energy may contribute to the heating of the corona. Red prominences can be seen on the west limb of the Sun as well as Earthshine on the Moon. The bright star Regulus (Alpha Leonis) is at top left, and magnitude 5.26 Nu Leonis is at right. Here the corona spans more than 5 solar radii and actually extends out of the field of view. The subtle and ethereal beauty of the corona, the Sun's outer atmosphere, is seen in a composite image of the total solar eclipse of August 21, 2017.