Turbulent Heating in the Fast Solar Wind

Details Turbulent Heating in the Fast Solar Wind Turbulent Heating in the Fast Solar Wind

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh52a..06d&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH52A-06

Physics

Plasma Physics

[7827] Space Plasma Physics / Kinetic And Mhd Theory, [7839] Space Plasma Physics / Nonlinear Phenomena, [7863] Space Plasma Physics / Turbulence, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

Nonlinear gyrokinetic simulations of Alfvenic and pseudo-Alfvenic turbulence in weakly collisional, magnetized turbulence have been carried out with the AstroGK code. Predictions of fluctuation spectra from earlier calculations [Howes, Dorland, et al., PRL 100:065004:2008] show good agreement with observations. The existence and character of the cascade of entropy (or free energy) at scales smaller than the gyroradius has been elucidated [Tatsuno, Dorland, et al., PRL 103:015003:2009]. Here, we examine the ion/electron heating ratio, with a particular focus on the fate of the energy of long wavelength pseudo-Alfvenic (or slow magnetosonic) waves. This energy is readily quantified by observation, as it is proportional to the power in the long wavelength density fluctuations. We attempt to connect the observed turbulent energy with the inferred plasma heating.

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