Quasilinear Dissipation and Focusing of Oblique Ion Cyclotron Waves by Coronal Hole Protons

Details Quasilinear Dissipation and Focusing of Oblique Ion Cyclotron Waves by Coronal Hole Protons Quasilinear Dissipation and Focusing of Oblique Ion Cyclotron Waves by Coronal Hole Protons

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh41c..03i&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH41C-03

Physics

2149 Mhd Waves And Turbulence (2752, 6050, 7836), 7511 Coronal Holes, 7827 Kinetic And Mhd Theory, 7863 Turbulence (4490), 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

Perpendicular proton heating in the low-beta solar coronal hole is observed by the UVCS/SOHO instrument and is likely responsible for the acceleration of the fast solar wind. Resonant cyclotron dissipation of turbulently generated Alfvén ion cyclotron waves is often invoked to provide this heating, but the necessary turbulent cascade of energy to resonant parallel scales is not understood. Additionally, Isenberg (2004) showed that dissipation of strictly parallel-propagating ion cyclotron waves is limited due to the presence of a marginally stable state of the proton distribution. In this talk, we demonstrate that proton absorption of oblique waves has no such limitation since it scatters the protons away from this marginal stability. We also find that the subsequently heated proton distribution will trend back to the stable state by emitting waves more aligned with the magnetic field. Thus, we present a mechanism which both heats protons and provides a quasilinear transport of turbulently generated oblique wavevectors toward the parallel direction. We report on our investigation to quantify and compare the effects of these two coupled processes in a coronal hole and in the solar wind.

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