NASA Scientists Observe the Sun in Different Wavelengths

This collage of solar images from NASA's Solar Dynamics Observatory (SDO) shows how observations of the sun in different wavelengths helps highlight different aspects of the sun's surface and atmosphere. 

The collage also includes images from other SDO instruments that display magnetic and Doppler information. 

Credit: NASA/SDO/Goddard Space Flight Center.

Taking a photo of the sun with a standard camera will provide a familiar image: a yellowish, featureless disk, perhaps coloured a bit more red when near the horizon since the light must travel through more of Earth's atmosphere and consequently loses blue wavelengths before getting to the camera's lens.

The sun, in fact, emits light in all coluors, but since yellow is the brightest wavelength from the sun, that is the colour we see with our naked eye -- which the camera represents, since one should never look directly at the sun. When all the visible colours are summed together, scientists call this "white light."

Specialist instruments, either in ground-based or space-based telescopes, however, can observe light far beyond the ranges visible to the naked eye.

Different wavelengths convey information about different components of the sun's surface and atmosphere, so scientists use them to paint a full picture of our constantly changing and varying star.

Yellow light of 5800 Angstroms, for example, generally emanates from material of about 10,000 degrees F (5700 degrees C), which represents the surface of the sun.

Extreme ultraviolet light of 94 Angstroms, on the other hand, comes from atoms that are about 11 million degrees F (6,300,000 degrees C) and is a good wavelength for looking at solar flares, which can reach such high temperatures.

By examining pictures of the sun in a variety of wavelengths - as is done through such telescopes as NASA's Solar Dynamics Observatory (SDO), NASA's Solar Terrestrial Relations Observatory (STEREO) and the ESA/NASA Solar and Heliospheric Observatory (SOHO) - scientists can track how particles and heat move through the sun's atmosphere.

We see the visible spectrum of light simply because the sun is made up of a hot gas - heat produces light just as it does in an incandescent light bulb but, when it comes to the shorter wavelengths, the sun sends out extreme ultraviolet light and x-rays because it is filled with many kinds of atoms, each of which give off light of a certain wavelength when they reach a certain temperature.

Not only does the sun contain many different atoms - helium, hydrogen, iron, for example -- but also different kinds of each atom with different electrical charges, known as ions.

Each ion can emit light at specific wavelengths when it reaches a particular temperature. Scientists have catalogued which atoms produce which wavelengths since the early 1900s, and the associations are well documented in lists that can take up hundreds of pages.

Solar telescopes make use of this wavelength information in two ways. For one, certain instruments, known as spectrometers, observe many wavelengths of light simultaneously and can measure how much of each wavelength of light is present.

This helps create a composite understanding of what temperature ranges are exhibited in the material around the sun. Spectrographs don't look like a typical picture, but instead are graphs that categorise the amount of each kind of light.