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Turbulence of an emitting gas in which the turbulent eddies are very small and unresolvable, giving rise to the broadening of a spectral line in a star's spectrum by Doppler shifts. If a Fraunhofer line is broader than expected from the motions of emitting atoms and other known causes, the excess broadening is sometimes attributed to unseen microturbulence, regardless of whether it actually exists.

Subjects: Astronomy and Astrophysics.

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