A narrow spectral feature records enhanced emission or absorption near a transition frequency. In a stellar atmosphere, its strength depends on atomic populations, opacity, velocity fields and the source function. Lines therefore diagnose composition as well as the physical atmosphere in which they form.
An emission line is a localized excess of specific intensity above the continuum. Heated chromospheric material can give a line source above the photospheric continuum source. Optically thin circumstellar gas can also add line photons through recombination or collisional excitation. Such line formation need not obey a thermal photospheric source prescription.
An absorption line is a deficit of observed spectral specific intensity relative to the surrounding continuum. In a photosphere with temperature falling outward, increased line opacity makes photons emerge from cooler layers than the continuum. For an absorption-dominated LTE source, the Planck function then supplies a smaller line specific intensity. A foreground layer with source below the incident continuum gives another direct transfer description.
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A spectral line is a dark or bright line in a spectrum, representing the absorption or emission of light at specific wavelengths by atoms or molecules. Spectral lines occur when electrons in an atom or molecule transition between energy levels; they either absorb or emit photons with wavelengths that correspond to the energy difference between those levels.
A single line in the emission spectrum.
Has been the leading motivation of the development of quantum mechanics, all the way from the:
- Schrödinger equation: major lines predicted, including Zeeman effect, but not finer line splits like fine structure
- Dirac equation: explains fine structure 2p spin split due to electron spin/orbit interactions, but not Lamb shift
- quantum electrodynamics: explains Lamb shift
- hyperfine structure: due to electron/nucleus spin interactions, offers a window into nuclear spin