Spectral Line

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Related to Stark broadening: Stark effect, pressure broadening

spectral line

[′spek·trəl ‚līn]
A discrete value of a quantity, such as frequency, wavelength, energy, or mass, whose spectrum is being investigated; one may observe a finite spread of values resulting from such factors as level width, Doppler broadening, and instrument imperfections. Also known as spectrum line.
McGraw-Hill Dictionary of Scientific & Technical Terms, 6E, Copyright © 2003 by The McGraw-Hill Companies, Inc.
The following article is from The Great Soviet Encyclopedia (1979). It might be outdated or ideologically biased.

Spectral Line


a thin line in an optical spectrum. Each such line can be characterized by a certain wavelength λ or frequency v = c/λ, where c is the speed of light. Spectral lines are observed in emission spectra as bright (colored) lines on a dark background and in absorption spectra as dark lines on a bright background. Each spectral line corresponds to a definite quantum transition in an atom, molecule, or crystal. Spectral lines are not strictly monochromatic: each one has a certain width Δλ.

The Great Soviet Encyclopedia, 3rd Edition (1970-1979). © 2010 The Gale Group, Inc. All rights reserved.
References in periodicals archive ?
Cardenosos, "New plasma diagnosis tables of hydrogen Stark broadening including ion dynamics," Journal of Physics B: Atomic, Molecular and Optical Physics, vol.
Stark broadening requires constraints on the electric field.
If Stark broadening mechanisms play any role in the Sun, it will only be in the context of condensed matter generating the associated electric field.
Stark broadening of [H.sub.[alpha]] line was used to estimate the electron temperature.
There are several possible mechanisms of line broadening in plasma: self-absorption, pressure broadening, Doppler broadening, Stark broadening, etc.
stated that Stark broadening may be one of the reasons since the broadening effect increases as the energy level increases [22].
Stark broadening of well-isolated lines in the plasma is, thus, useful for estimating the electron number densities provided that the Stark-broadening coefficients have been measured or calculated.
Both ions and electrons induce Stark broadening, but electrons are responsible for the major part because of their higher relative velocities.
W is the electron impact parameter (stark broadening value) and it is given in Table 2).