Spectral linewidth refers to the width of a spectral line, representing the range of frequencies or wavelengths over which a particular transition occurs. It is influenced by factors such as natural broadening, Doppler broadening, and pressure broadening, and is crucial for understanding the precision and resolution of spectroscopic measurements.

Spectral Linewidth

Spectral linewidth

width of a spectral line

range of frequencies

wavelengths over which a particular transition occurs

Natural broadening is an intrinsic line broadening mechanism in spectral lines caused by the finite lifetime of excited states, leading to an uncertainty in energy levels as described by the Heisenberg uncertainty principle. It is an inherent property of atoms and molecules, independent of external perturbations, and results in a Lorentzian line shape in spectral analysis.

natural broadening

Doppler broadening is a phenomenon observed in spectral lines, caused by the relative motion between the source of light and the observer, which leads to a spread in the frequency of emitted or absorbed light. This effect is significant in various fields such as astrophysics and plasma physics, where it helps in determining the temperature and velocity distribution of particles in a medium.

Doppler broadening

Pressure broadening is a phenomenon where spectral lines are broadened due to collisions between particles in a gas, affecting the energy levels of the emitting or absorbing species. This effect is significant in environments with high pressure, such as stellar atmospheres and laboratory plasmas, and is crucial for interpreting spectroscopic data accurately.

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