Astrophysics (index)

Spectral Line

(dark or light line in a spectrum)

A Spectral Line is a dark or light line in a Continuous Spectrum. For example, the Magnitude of different Wavelengths of light from something may generally be described curve, i.e., nearby wavelengths have nearly the same magnitude. A line would be an exception to this, i.e., a "spike" indicating a wavelength at which light has a much higher magnitude than nearby wavelengths, or a dip where a wavelength has a much lower magnitude than nearby wavelengths.

Light lines are generally caused by Emissions at specific wavelengths (Emission Lines), and dark lines are caused by Absorption at specific wavelengths (Absorption Lines). Lines are related to chemical makeup of the light source or absorber, indicating changes of energy level of electrons, which have characteristic values based upon chemistry.

Characteristics of the details of lines can show other characteristics of the light source or intervening absorber such as velocity, Turbulence, etc.

Among the widely used spectral lines are the Hydrogen (H) series of lines, e.g.,

Atomic spectral lines are sometimes classified by element and ionization, specified by the chemical symbol followed by a Roman numeral, I meaning neutral, II meaning singly ionized positive, III meaning doubly ionized, etc.

The term Line Broadening refers to the mechanisms that create the shape of a line, e.g., in Electromagnetic Radiation (EMR) from a star.

Spectral-Line Mapping refers to imaging or surveying a portion of the sky for the presence of particular spectral lines, often noting their Redshift (z), to determine their Radial Velocity. Its uses include investigations of Accretion Disks, Jets, Molecular Clouds, the entire Milky Way, and other galaxies.


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

Referenced by:
Absorption
Absorption Line
Balmer Jump
Balmer Series
Bohr Model
Brackett Series
Calcium-Rich Gap Transient
Carbon (C)
Carbon Monoxide (CO)
Cold Gas
Continuous Absorption
Continuous Spectrum
Continuum Emission
Convolution
Core Collapse Supernova
C+
DeGaS-MC
Degeneracy
Velocity Dispersion (σ)
Doppler Broadening
Double-Line Spectroscopic Binary
Electron Orbital
Emission Line
EMPIRE Survey
Fine Structure
Forbidden Line
Full Width At Half Maximum (FWHM)
H-alpha (Ha)
HI Region (HI)
Hydrogen (H)
Hyperfine Structure
Intensity Mapping
Interferometer
K Correction
Kepler Radius
Kinematic Distance
Kirchhoff's Laws
Lyman-Alpha Emitter (LAE)
Line Broadening
Line Shape Function
Lyman Alpha (Ly-α)
Lyman-Alpha Forest
Lyman Series
Molecular Cloud
Molecular Deep Field
Nitrogen (N)
Oxygen Lines
Paschen Series
PAWS
Position-Position-Velocity Space (PPV)
Radial Velocity
Redshift (z)
R-Process
Silicon (Si)
Spectral Line Energy Distribution (SLED)
Supernova (SN)
Sobolev Approximation
Spectral Band
Spectral Class
Spectroscope
Spectroscopic Binary
State of Excitation
State of Ionization
Stellar Model Atmosphere
Sulfur (S)
Surface Abundance
Surface Temperature
Tully-Fisher Relation (TFR)
Tomographic Ionized-Carbon Mapping Experiment (TIME)
21cm Line
Turbulence
Type Ia Supernova
Water Lines
White Dwarf
CO to H2 Factor (Xco)
Zeeman-Doppler Imaging (ZDI)

index