An absorption line will appear in a spectrum if an absorbing material is placed between a source and the observer. This material could be the outer layers of a star, a cloud of interstellar gas or a cloud of dust.
: a more or less narrow range of wavelengths in a spectrum that is darker than neighboring wavelengths. s are seen in stars.
A dark line in a spectrum that represents the absorption of energy at a particular wavelength of light. Each element on the periodic table absorbs energy at unique wavelengths.
: A dark line in a spectrum; produced by the absence of photons absorbed by atoms or molecules.
absorption spectrum (dark-line spectrum): A spectrum that contains s.
absorption line spectrum
Dark lines superimposed on a continuous spectrum.
The rate at which an object's velocity changes due to a change in speed, a change in direction, or both.
A narrow dark line within a spectrum. It is caused by specific gases absorbing a portion of radiation, and its width represents the relative abundance of the gases.
Absorption line: A dark line or band at a particular wavelength on a spectrum, formed when a substance between a radiating source and an observer absorbs electromagnetic radiation of that wavelength.
. A break of depression in a continuous spectrum caused by the absorption of photons within narrow wavelengths by some types of atom, ion, or molecule.
Absorption Line - A dark line superimposed on a continuous spectrum when a gas absorbs light from a continuous source that is hotter than the absorbing gas ...
When sunlight is split by a prism, at first glance it appears to produce a continuous spectrum.
ABSORPTION LINE - Narrow range of wavelengths in a spectrum that are darker (have lower intensity) than neighboring wavelengths.
s Dark lines interrupting a continuous color spectrum, caused by a cool gas between the light source and the observer. Cool gas absorbs light in the same frequencies as it emits when hot, e.g. double yellow line of sodium.
Dark lines in a spectrum, produced when light or other electromagnetic radiation coming from a distant source passes through a gas cloud or similar object closer to the observer.
An is produced when a photon of just the right energy is absorbed by an atom, kicking an electron to a higher energy orbit. The photon had energy = the difference in energy of the energy orbits.
Absorption lines of KrI
No Kr line is seen in the solar spectrum.
Absorption lines of KrII
Following Bidelman's (1960) discovery of KrII in 3 Cen A, this element was observed in some other hot Bp stars. W(4355) = 0.025 according to Hardorp (1966).
A dark line in a continuous spectrum caused by absorption of light.
A spectral line is a dark or bright line in an otherwise uniform and continuous spectrum, resulting from an excess or deficiency of photons in a narrow frequency range, compared with the nearby frequencies.
s: Dark lines superimposed over a bright continuous spectrum background, created when a cooler gas absorbs photons from a hotter source.
Absorption lines against a continuous spectrum are seen as the photons emitted at particular wavelengths are emitted in all directions, so would produce a dark line.
In spectroscopy, and in particular the solar Fraunhofer spectrum, a characteristic wavelength of emitted radiation that is partially absorbed by the medium between the source and the observer.
Narrow spectral features that represent a reduction in intensity over a small wavelength range. They are caused by the loss of photons that raise an atom from a particular energy state to a higher energy state.
absorption spectrum ...
s are dark lines superimposed over a bright continuous absorption spectrum. Each dark line is formed as a cooler gas absorbs photons emitted by a particular element from a hotter source.
The absorption line of neutral calcium at 4227 Angstroms is thus strong in cool M-type dwarf stars, in which the pressure is high and the temperature is low.
The s of a solar or other stellar spectrum.
frequency - (n.) ...
Dark absorption lines in the sun's spectrum and that of other stars are called Fraunhofer lines after Joseph von Fraunhofer (1787-1826) who observed them in 1817.
Broad s are direct evidence of outflow from AGNs, at very respectable velocities.
Emission and absorption lines in radio astronomy usually originate from atoms and small molecules or molecular ions in gaseous form, and molecular transitions at radio wavelengths are usually rotational.
Search for s from the evaporated atmosphere of extrasolar planets in the visible.
April 7, 2007 COUSTENIS A., MAYOR M., SCHNEIDER J., QUELOZ D. & EGGENBERGER A.
Relatively few absorption lines. Lines of ionized helium and other lines of highly ionized atoms. Hydrogen lines appear only weakly. Peak of light in UV part of spectrum.
(NASA SP-7, 1965) A minute range of wavelength (or frequency) in the electromagnetic spectrum within which radiant energy is absorbed by the medium through which it is passing.
absorption line The absence or reduction of radiation at one or several adjacent wavelengths in a continuous spectrum.
A certain that is found at 5000 Angstroms in the lab is found at 5050 Angstroms when analyzing the spectrum of a particular galaxy.
H-alpha. This absorption line of neutral hydrogen falls in the red part of the visible spectrum and is convenient for solar observations. The H-alpha line is universally used for observations of solar flares.
See also: Spectrum, Astro, Solar, Star, Sun