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Context. Red supergiants are observed to undergo vigorous mass-loss. However,to date, no theoretical model has succeeded in explaining the origins of theseobjects' winds. This strongly limits our understanding of red supergiantevolution and Type II-P and II-L supernova progenitor properties.  Aims. We examine the role that vigorous atmospheric turbulence may play ininitiating and determining the mass-loss rates of red supergiant stars.  Methods. We analytically and numerically solve the equations of conservationof mass and momentum, which we later couple to an atmospheric temperaturestructure, to obtain theoretically motivated mass-loss rates. We then comparethese to state-of-the-art empirical mass-loss rate scaling formulae as well asobservationally inferred mass-loss rates of red supergiants.  Results. We find that the pressure due to the characteristic turbulentvelocities inferred for red supergiants is sufficient to explain the mass-lossrates of these objects in the absence of the normally employed opacity fromcircumstellar dust. Motivated by this initial success, we provide a firsttheoretical and fully analytic mass-loss rate prescription for red supergiants.We conclude by highlighting some intriguing possible implications of theserates for future studies of stellar evolution, especially in light of the lackof a direct dependence on metallicity.

Analytic, dust-independent mass-loss rates for red supergiant winds initiated by turbulent pressure