Above , filament and prominence ; below , spectrum of visible light
COURTESY OF Debasis Sarkar and Janmejoy Sarkar . ( Sky Watchers Association of North Bengal ) viewing systems also give stunning views of solar eclipses . Shooting this giant blazing ball during transits of inner planets or the International Space Station over its face is also a fascinating challenge for serious sky enthusiasts .
What is the colour of sunlight ? The Sun releases a huge bundle of electromagnetic waves of a wide range of wave lengths . Out of this complete range or spectrum , only a tiny portion from red to violet comes within our visual perception . While red has its wavelength of 700 Nanometer or 7000 Angstroms ( Å = 1 /, 00,00,000 millimeter ), that of violet is 400 nm or 4000 Å . Thus , when this almost white incidental is broken down using a prism , it gives an output as a wide band of different colours from red to violet . This is a smaller portion of the full spectrum of visible light in different colours . Each colour in that spectrum has its own distinctive wavelength .
How bright is the Sun ? It is absolutely too bright to be seen . The first objective in observing is to reduce the intensity of sunlight .
This is done using Sun filters that can bring down the intensity to 1 / 100,000 times . At this diminished intensity , the Sun appears no brighter than the Full Moon . As all the colours of sunlight get almost equally attenuated with these filters , we find the Sun as a near white dish . But it appears almost flat and featureless as details of the Sun ’ s
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