Perpendicular Ion Heating in Low-frequency Alfvén-wave Turbulence

Details Perpendicular Ion Heating in Low-frequency Alfvén-wave Turbulence Perpendicular Ion Heating in Low-frequency Alfvén-wave Turbulence

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43c1974x&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43C-1974

Physics

Plasma Physics

[7845] Space Plasma Physics / Particle Acceleration, [7863] Space Plasma Physics / Turbulence

Scientific paper

Determining the mechanism that heats the solar corona is a fundamental problem in heliospheric physics. One of the proposed models is based on low-frequency Alfvén waves (ω << Ωi ) launched from the coronal base. In the low-β corona where the magnetic field is strong, MHD studies show that Alfvén wave turbulence primarily cascades to smaller scales perpendicular to the mean magnetic field rather than the parallel direction. Chandran et al 2010 studied the possibility of ion heating by this low-frequency Alfvén-wave turbulence: In low-β plasma, when the particle's gyro-radius is comparable to the wave length in the perpendicular direction, the ion undergoes a random walk in the time-varying electrostatic potential. When the fluctuation amplitude exceeds a threshold, this stochastic mechanism could provide ion heating in the plane perpendicular to the magnetic field lines. In this work, we run particle simulations in a more realistic RMHD field, which can not be described by simple wave conception. We study ions' behavior in a fully turbulent regime and re-evaluate some important parameters in the previous theory.

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