A spectrograph measures how bright a star is at any given wavelength.
These characteristics are exploited in making semiconductor lasers that produce light of any given wavelength within a considerable range.
The change in energy as the wave passes through a layer is a constant of the material for a given wavelength and is called its absorption coefficient.
The figure shows a ray of ordinary (nonpolarized) light of a given wavelength incident on a reflecting surface of a transparent medium (e.g., water or glass).
Thus for radiation of a given wavelength, an infinitesimally thin layer will reduce the energy of a wave by a fractional amount that is proportional to the thickness of the layer.
Line radiation is emitted at only one specific wavelength (like an optical spectral line), and so its detection requires that a radio telescope be set at precisely that given wavelength.
Those are composed of a continuous arrangement of submirrors reflecting each one at a given wavelength.
Additionally, the frequency for a given wavelength can be shifted by the magnetic field.
The "phase velocity" describes how fast waves of a given wavelength move, and the "group velocity" describes how fast the light conveys energy or information.
The Group Velocity Dispersion (GVD) of HC-PCF can be compensated at a given wavelength by scaling the fiber dimensions.
While the spectra of different samples can be very similar at given wavelength, the wavelength dependence should be considered for correlating spectral features to crystallite size La.
