Generation of the Fast Solar Wind by Obliquely-Propagating Ion Cyclotron Waves

Details Generation of the Fast Solar Wind by Obliquely-Propagating Ion Cyclotron Waves Generation of the Fast Solar Wind by Obliquely-Propagating Ion Cyclotron Waves

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh44a..06i&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH44A-06

Physics

Plasma Physics

[2169] Interplanetary Physics / Solar Wind Sources, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7827] Space Plasma Physics / Kinetic And Mhd Theory, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

The fast solar wind results from strong proton heating in coronal holes. The primary heating is perpendicular to the magnetic field and it is broadly distributed over the first 4 - 5 solar radii. Such perpendicular ion heating is a basic consequence of the resonant cyclotron dissipation of ion cyclotron waves, which can also naturally explain the observed preferential energization of heavy ions. However, Isenberg [JGR, 109, 3101, 2004] showed that strictly parallel-propagating waves, which were often invoked at the time, are limited in their ability to heat protons through cyclotron resonance. These waves could not, on their own, drive a fast solar wind. This limitation does not exist for the more realistic case which considers waves over a finite range of propagation angles. We have modeled the quasilinear resonant diffusion of coronal hole protons, assuming plausible resonant wave intensities along with the kinetic effects of large-scale external forces. We will describe this model and report on the heating, acceleration and detailed kinetic proton distributions which result.

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