absorption lines


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ab·sorp·tion lines

the dark lines in the solar spectrum corresponding to wavelengths originally emitted by inner layers of the Sun but then absorbed by various elements present in gaseous form in cooler layers and in the Earth's atmosphere.
Synonym(s): Fraunhofer lines

ab·sorp·tion lines

(ăb-sōrp'shŭn līnz)
Dark lines in the solar spectrum due to absorption by the solar and the earth's atmosphere.

absorption lines

In spectroscopy, dark lines of the solar spectrum.
References in periodicals archive ?
Once you are proficient at analyzing the absorption lines of stars, you might try examining the emission lines of nebulae.
The strength of the emission lines decreases and absorption lines of singly ionized metals get stronger from 2010 to 2013.
Because we do not know the distance and temperature of the X-ray absorbing cloud and the degree of ionization of the oxygen atoms, the exact wavelengths of the absorption lines are not known a priori.
The quantities [[PHI].sub.0] and [PHI] are the incident and the transmitted radiant powers; [S.sub.T] is the molecular transition line strength of the probed absorption line at gas temperature T which is matched to the actually present isotopic abundance by means of [r.sub.iso], which is the ratio of the abundance in the sample compared to the value for which the line strength is reported.
Two absorption lines at 3191 and 3347 [cm.sup.-1] are due to hydrogen-nitrogen stretching as revealed by DFT calculations.
The cosmic gas selectively absorbs light at very specific frequencies which astronomers refer to as "absorption lines." The pattern and shape of these lines provide a cosmic barcode, which astronomers can decode to determine the chemical composition, density, and temperature of the gas.
However, special measurement techniques have to be applied when weak absorption lines are utilized.
Spectroscopic observations map the Mrk 509 warm absorber, study the mini-broad absorption line quasar PG 1126-041, determine the source of reddening in low ionization BAL quasars, and probe quasar winds using narrow intrinsic absorption lines.
Atomic and molecular absorption lines are very stable under changing environmental conditions and are excellent references for this purpose.
Characteristic narrow absorption lines, observed at 380 and 435 nm, are most likely from forbidden spin transitions in ferrous iron.
We have analyzed Fe 11 absorption lines toward several of the reddened stars included in the FUSE survey of molecular hydrogen abundances in translucent clouds.
So, when patterns of dark absorption lines with just those spacings show up in the spectra of quasars, astronomers conclude that an intervening gas cloud contains particular types of atoms.