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Introduction
Most readers acquainted with the hydrogen spectrum  will be familiar with the set of lines in the visible spectrum representing transitions of electrons from energy levels 3,4,5 and 6 (H alpha, beta, gamma and delta respectively)  of atomic hydrogen to energy level 2 – the Balmer series lines. The picture below shows 3 of these lines (amongst others) in a diffraction grating image of the solar chromosphere during a total eclipse of the sun. For a very brief moment the normal dark Fraunhofer lines of the solar absorption spectrum become an emission spectrum. The diffraction grating then shows separated images of the eclipse at  various prominent wavelengths (indicated in the diagram) within the chromospheric emission spectrum. See also: The Spectrum of the...


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