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These lines are representative of the elements present in the atmosphere of the star.

The measurement and study of absolute infrared absorption intensities

Type I: supernovae WITHOUT hydrogen absorption lines in their spectrum

Since that time interstellar absorption lines have been recorded in the spectra of many stars.

Emission can occur at any frequency at which absorption can occur, and this allows the absorption lines to be determined from an emission spectrum.

It is the depth of the absorption lines that contains the information on CO2 concentration.

For the same element, the absorption lines correspond to the emission lines (see the two spectra for lithium at the bottom of the right image).

The emission lines are the lines of colors on black background, issued by the observed objet that the absorption lines are black stripes on iridescent background, so the colors absorbed by objects crossed by the light.

Technetium star – Star whose stellar spectrum contains absorption lines of technetium

DBV (GCVS: ZZB) DB spectral type, having only helium absorption lines in its spectrum

We can see that the peaks of absorption are indeed lower but the widths of the absorption lines are wider (for the surface results).

The emission lines and absorption lines represent the energy levels of atoms and therefore the atoms themselves, present in the layers crossed by the light.

DAV (GCVS: ZZA) DA spectral type, having only hydrogen absorption lines in its spectrum

Due to the exotic nature of its spectrum (bright emission lines in lieu of dark absorption lines) it is dubbed the "Spectral Gem of the Southern Skies".