How SDO Sees the Sun?

These images show the different ways the Solar Dynamics Observatory views the sun using the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) onboard the spacecraft.
Starting at the top left and moving across and then down:
1700: Ultraviolet light continuum, shows surface of the sun. As well as a layer of the sun's atmosphere called the chromosphere.
4500: White light continuum, shows the sun's surface or photosphere.
1600: Emitted by carbon-4 (C IV) at around 10,000 K. C IV at these temperatures is present in what's called the transition region between the sun's surface and the lowest levels of the sun's atmosphere, the chromosphere and are typically colorized in dark yellow.
304: Emitted by helium-2 (He II) at around 50,000 K. This light is emitted from the upper transition region and the chromosphere and are typically colorized in red.
171: Emitted by iron-9 (Fe IX) at around 600,000 K. This wavelength shows the quiet corona and coronal loops, and is typically colorized in gold.
193: Emitted by iron-12 (Fe XII) at 1,000,000 K and iron 24 (Fe XXIV) at 20,000,000 K. The former represents a slightly higher region of the corona and the later represents the much hotter material of a solar flare. This wavelength is typically colorized in yellow.
211: Emitted by iron-14 (Fe XIV) at temperatures of 2,000,000 K. These images show hotter, active regions in the sun's corona and are typically colorized in purple.
335: Emitted by iron-16 (Fe XVI) at temperatures of 2,500,000 K. These images also show active regions in the corona, and are typically colorized in blue.
94: Emitted by iron-18 (Fe XVIII) at temperatures of 6,000,000 K. Temperatures like this represent regions of the corona during a solar flare. The images are typically colorized in green.
131: Emitted by iron-20 (Fe XX) and iron-23 (Fe XXIII) at temperatures greater than 10,000,000 K, representing the material in flares. The images are typically colorized in teal.
Credit: NASA/SDO

Page Last Updated: November 20th, 2014
Page Editor: Holly Zell