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Total Solar Eclipse Corona - Solarized

On August 21, 2017 the path of the first solar eclipses over the Unites States in 38 years traversed approximately 2,500 miles of the country from Newport, Oregon to McClellanville, South Carolina. Just outside Shoshoni, Wyoming, the path passed over Boysen Reservoir. At this location, totality lasted 2 minutes and 22 seconds, being at its maximum about 11:40 am. With the moon blocking the solar disk during totality, red flares called solar prominences become visible at the edge of the dark disk. The red-glowing looped material is plasma, a hot gas composed of electrically charged hydrogen and helium. These prominences look small in relation to the size of the sun, but typically extend over many thousands of kilometers with the largest on record being estimated at over 800,000 kilometres (500,000 miles). A prominence forms over timescales of about a day and may persist for several weeks or months.

During the total solar eclipse, the sun’s outer atmosphere called the corona becomes visible as it extends millions of miles into space. The corona consists of extremely hot ionized gases which exceed 1 million degrees Kelvin – 150- to 450-times hotter than the surface of the sun. Being over 1 million million times less dense and much hotter than the sun’s surface and the solar prominences, the corona actually produces about one-millionth as much visible light, thus becoming visible from earth typically only during a total solar eclipse. The sun’s magnetic fields bend the corona into its remarkable shapes.

In this image, 10 different photographic exposures of the solar eclipse were composited to show the eclipsing moon, solar prominences and the corona. The image was then manipulated by a process called embossing where each pixel is replaced either by a highlight or a shadow, depending on light/dark boundaries on the original image. The final image represents the rate of color change at each location of the original. This approach accentuates the pattern

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Filename
total-solar-eclipse-sun-corona-solarized.tif
Copyright
Copyright © Lloyd Paul Aiello
Image Size
7360x4912 / 69.9MB
www.WildernessPortraits.com
Contained in galleries
Digitally Manipulated, Clouds and Sky, Recent Additions, Abstractions
On August 21, 2017 the path of the first solar eclipses over the Unites States in 38 years traversed approximately 2,500 miles of the country from Newport, Oregon to McClellanville, South Carolina. Just outside Shoshoni, Wyoming, the path passed over Boysen Reservoir. At this location, totality lasted 2 minutes and 22 seconds, being at its maximum about 11:40 am. With the moon blocking the solar disk during totality, red flares called solar prominences become visible at the edge of the dark disk. The red-glowing looped material is plasma, a hot gas composed of electrically charged hydrogen and helium. These prominences look small in relation to the size of the sun, but typically extend over many thousands of kilometers with the largest on record being estimated at over 800,000 kilometres (500,000 miles). A prominence forms over timescales of about a day and may persist for several weeks or months.<br /> <br /> During the total solar eclipse, the sun’s outer atmosphere called the corona becomes visible as it extends millions of miles into space. The corona consists of extremely hot ionized gases which exceed 1 million degrees Kelvin – 150- to 450-times hotter than the surface of the sun. Being over 1 million million times less dense and much hotter than the sun’s surface and the solar prominences, the corona actually produces about one-millionth as much visible light, thus becoming visible from earth typically only during a total solar eclipse. The sun’s magnetic fields bend the corona into its remarkable shapes.<br /> <br /> In this image, 10 different photographic exposures of the solar eclipse were composited to show the eclipsing moon, solar prominences and the corona. The image was then manipulated by a process called embossing where each pixel is replaced either by a highlight or a shadow, depending on light/dark boundaries on the original image. The final image represents the rate of color change at each location of the original. This approach accentuates the pattern