- Conference date: 17-31 June 2002
- Location: Pisa (Italy)
We present a model of the resonant cyclotron dissipation of parallel‐propagating ion‐cyclotron waves in a coronal hole under the kinetic shell approximation. This approximation takes the resonant quasilinear wave‐particle interaction to be much faster than the non‐resonant processes affecting the proton distribution, essentially maintaining the resonant protons in a state of marginal stability with respect to this wave mode. Thus, the kinetic shell model represents the case of maximum possible dissipation by the resonant cyclotron mechanism. When the additional simplification of dispersionless waves is made, this model easily yields fast solar wind flows from plausible conditions at the model inner boundary. However, when ion‐cyclotron dispersion is included the model fails, resulting in cooling of the proton population and weak acceleration to speeds on the order of 300 km s−1. We conclude that resonant dissipation of parallel‐propagating waves cannot be responsible for the fast solar wind.
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