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Spectra of a Metal-Poor and a Metal-Rich Star

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Description
Spectra of a Metal-Poor and a Metal-Rich Star
These spectra compare (a) a metal-poor (Population II) and (b) a metal-rich (Population I) star (the Sun) of the same surface
temperature. Numerous spectral lines prominent in the solar spectrum are caused by elements heavier than hydrogen and
helium. Note that corresponding lines in the metal-poor star’s spectrum are weak or absent. Both spectra cover a wavelength
range that includes two strong hydrogen absorption lines, labeled Hγ (410 nm) and Hδ (434 nm).
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