Astrophysics (index)about

Absorption Line

(dark line in a spectrum)

An Absorption Line is a Spectral Line due to Absorption of a specific Wavelength within a Continuous Spectrum of Electromagnetic Radiation that is passing through a transparent medium such as a cloud or Atmosphere. The lines occur due to a preference of atoms to absorb radiation at specific Frequencies that match the energy level of transitions to an increased level of Atomic Excitation. The lines reveal information both about the makeup of the gas and its Temperature.

Per Kirchhoff's Laws, absorption lines indicate a cooler gas in front of a hotter source of radiation, presumably an approximate Black Body. One case of such "cooler gas" is the Photosphere of stars, and absorption lines are the basis for stellar Spectral Classes.

By contrast, Emission Lines are produced when a thin gas has sufficient atomic excitation that relaxation to lower levels is a significant source of its radiation.

For some phenomena, both absorption and Emission lines are observed for an Element, e.g., for supernovae, if some gas is blown away initially sufficiently energetic to produce emission lines, and later cooler and in front of a hotter material closer to the supernova center.

Telluric Lines are absorption lines from the Earth's atmosphere, and are a challenge to carrying out Spectrography on the ground (Telluric Contamination).


(lines,spectrum)
http://en.wikipedia.org/wiki/Spectral_line

Referenced by:
Absorption
A-Type Star (A)
Atomic Excitation
B-Type Star (B)
Be Star
Calcium (Ca)
Continuous Absorption
Emission Line Galaxy (ELG)
Emission Line
F-Type Star (F)
G Band
G-Type Star (G)
GJ 1214 b
Gunn-Peterson Trough
Interstellar Medium (ISM)
Kirchhoff's Laws
L-Type Star (L)
Line Blanketing
Line Broadening
Line Shape Function
Lyman-Alpha Forest
M-Type Star (M)
O-Type Star (O)
Schuster-Schwarzschild Model
Supernova (SN)
Spectral Line
Titan
21cm Line
Transiting Planet
Two-stream Approximation
Water Lines
Zeeman-Doppler Imaging (ZDI)

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