Computer Science
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..629v&link_type=abstract
MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp
Computer Science
Plasma Alfven Waves, Dusty Plasmas, Supergiant Stars, Stellar Winds, Magnetohydrodynamics And Plasmas, Magnetohydrodynamic Waves, Dusty Or Complex Plasmas, Plasma Crystals, Supergiant Stars, Mass Loss And Stellar Winds
Scientific paper
One of the most promising mechanisms that drive the winds of cool supergiant stars involves an outward-directed flux of Alfvén waves. This mechanism can explain both the high mass-loss rate and the low terminal velocities of these winds. Many models were proposed using Alfvén waves damping mechanisms such as surface resonant, non-linear, turbulent, or assuming a constant damping length. Since it is observed that late-type stars present great quantities of dust particles in their winds, we propose a damping mechanism for the waves that is caused due to their interaction with dust grains: the dust-cyclotron damping. We assume that particles are distributed over a range of sizes, implying a broad band of resonance frequencies. Our results show that this damping mechanism can accelerate the wind and reproduce observational data of cool supergiant stars, such as the mass-loss rate and the terminal velocity.
Jatenco-Pereira Vera
Vidotto Aline A.
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