An energy peak in a continuous spectrum caused by the emission of those photons by the de-excitation of electrons in atoms.
Bright line in a specific location of the spectrum of radiating material, corresponding to emission of light at a certain frequency.
a more or less narrow range of wavelengths in a spectrum that is brighter than neighboring wavelengths. Emission lines are seen in quasars.
a bright band at a particular wavelength on a spectrum, emitted by the source and indicating by its wavelength a chemical constituent of that source.
A discrete bright line in the spectrum.
A bright line in a spectrum caused by the emission of photons from atoms.
Within a spectrum, an excess amount of energy that is emitted at a specific wavelength. Emission lines in a spectrum usually appear as slender slivers of light on a dark background. The extra light at these wavelengths results from an electron "falling" from a high atomic energy state to a lower energy state. When this happens, the atom emits a photon, or discrete unit of energy in the form of light. The difference in energy between the two energy states determines the wavelength and frequency (color) of the emission line. An absorption line is just the opposite of an emission line. Instead of emitting a photon, an absorption line represents an atom absorbing a photon at a specific wavelength and energy. In a spectrum, absorption lines appear as darkened slivers, where light is missing from the spectrum. See also absorption line spectral line
A bright section of a spectrum at a particular wavelength. Usually emitted by a hot gas.
A line of finite width in the emission spectrum, characteristic of gaseous emission. Emission lines are characterized by their central wavelength, line intensity, and line width.
A bright line in a spectrum caused by emission of light. Each chemical element emits and absorbs radiated energy at specific wavelengths. The collection of emission lines in a spectrum corresponds to the chemical elements contained in a celestial object.