As soon as stellar spectra were analyzed spectroscopically in the second half of the nineteenth century, it became clear that these spectra exhibit a bewildering variety. The need for some order, or rather some ‘classification’, became urgent. Of the many schemes suggested for stellar classification, the Harvard scheme, proposed by Pickering, was accepted in 1910 as the standard.
Spectral Line Solar Atmosphere Main Sequence Equivalent Width Main Sequence Star
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