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There are in the literature several theories to explain the mass loss instellar winds. In particular, for late-type stars, some authors have proposed awind model driven by an outward-directed flux of damped Alfven waves. The windsof these stars present great amounts of dust particles that, if charged, cangive rise to new wave modes or modify the pre-existing ones. In this work, westudy how the dust can affect the propagation of Alfven waves in these windstaking into account a specific damping mechanism, dust-cyclotron damping. Thisdamping affects the Alfven wave propagation near the dust-cyclotron frequency.Hence, if we assume a dust size distribution, the damping occurs over a broadband of wave frequencies. In this work, we present a model of Alfvenwave-driven winds using the dust-cyclotron damping mechanism. On the basis ofcoronal holes in the Sun, which present a superradial expansion, our model alsoassumes a diverging geometry for the magnetic field. Thus, the mass, momentum,and energy equations are obtained and then solved in a self-consistentapproach. Our results of wind velocity and temperature profiles for a typicalK5 supergiant star shows compatibility with observations. We also show that,considering the presence of charged dust particles, the wave flux is lessdamped due to the dust-cyclotron damping than it would be if we consider someother damping mechanisms studied in the literature, such as nonlinear damping,resonant surface damping, and turbulent damping.

The Effects of Alfven Waves and Radiation Pressure in Dusty Winds of Late‐Type Stars. II. Dust‐Cyclotron Damping