emission lines


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emission lines

See emission spectrum.
Collins Dictionary of Astronomy © Market House Books Ltd, 2006

emission lines

[i′mish·ən ‚līnz]
(spectroscopy)
Spectral lines resulting from emission of electromagnetic radiation by atoms, ions, or molecules during changes from excited states to states of lower energy.
McGraw-Hill Dictionary of Scientific & Technical Terms, 6E, Copyright © 2003 by The McGraw-Hill Companies, Inc.
References in periodicals archive ?
As the supermassive black hole actively consumes matter from its accretion disk, it drives the AGN to create two regions, one that produces broad emission lines, and another that produces narrow emission lines.
The pulse energy employed was 25 mJ approximately, because using a higher energy than this value caused saturation in emission lines.
The wavelengths of these coronal emission lines did not match those from elements known in the 19th century, and their origin had been a mystery.
The observed lines of resonance Raman scattering and possible combination of phonons responsible for these emission lines are presented in Tables 1 and 2.
In theory, taking a ratio of two emission lines can compensate for the fluctuations in the amplitude of spectra caused by experimental conditions.
Contrary to the SSM which advocates that emitting species must first be excited through the interaction with light, followed by re-emission disconnected from chemical processes, the LMHSM proposes that all emission lines are inherently linked to chemical or electrical processes in the Sun [23-27].
The strength of the emission lines decreases and absorption lines of singly ionized metals get stronger from 2010 to 2013.
The Balmer emission lines (labelled H[alpha] to H[beta]) from the ionised hydrogen gas in the disc were relatively weak at the peak of the outburst with several of the lines immersed in broad absorption features caused by the opacity of the dense, hot gas in the disc.
The goal of the research group is to establish a new exploration method using as reference various molecular/atomic emission lines which can be observed at millimeter/submillimeter wavelengths.
By analyzing the ammonia (NH3) (1,1) and (2,2) emission lines in G22.56-0.2 we were able to determine the physical properties of the IRDC.
Other topics include relativistic winds from supermassive black holes, gas kinematics in the inner few hundred parsecs of NGC 1068, and the effects of an accretion disk wind on the profile of AGN emission lines. Most of the papers are collaborations across multiple universities.
The database of IR/optical/UV emission lines from low-ionization nuclear emission regions (LINERs) is very extensive and advanced.

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