Ion-cyclotron Resonance with Streaming Bi-Maxwellian Distribution

Abstract

We investigate the effect of bulk velocity of the solar wind on the propagation characteristics of ion-cyclotron waves (ICWs). Our model is based on the kinetic theory. We solve the Vlasov equation for O VI ions and obtain the dispersion relation of ICWs. Refractive index of the medium for a streaming bi-Maxwellian velocity distribution proved to be higher than that of the bi-Maxwellian velocity distribution. The bulk velocity of the solar polar coronal holes' plasma increases the value of the refractive index by a factor of 1.5 (3) when the residual contribution is included (neglected). The ratio of the refractive index of interplume lanes to the plume lanes at the coronal base is also higher than we found for the bi-Maxwellian velocity distribution, i.e. $k_{interplume}/k_{plume}=2.5$.

15 pages, 3 figures, New Astronomy accepted

References in corpus (5)

• Connecting the Sun and the Solar Wind: The First 2.5 Dimensional Self-consistent MHD Simulation under the Alfvén Wave Scenario
• On the origin of the 1/f spectrum in the solar wind magnetic field
• Evidence of Wave Damping at Low Heights in a Polar Coronal Hole
• Improved Constraints on the Preferential Heating and Acceleration of Oxygen Ions in the Extended Solar Corona
• Ion-cyclotron waves in Solar Coronal Hole