Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh53a1288g&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH53A-1288
Physics
Plasma Physics
[2159] Interplanetary Physics / Plasma Waves And Turbulence, [7829] Space Plasma Physics / Kinetic Waves And Instabilities, [7859] Space Plasma Physics / Transport Processes
Scientific paper
The inertial range of solar wind turbulence corresponds to magnetic power spectra which scale approximately as f^{-5/3}. Many observations show, however, that at observed frequencies greater than about 0.2 Hz, there is a "breakpoint" such that power spectra at higher frequencies follow a steeper power-law dependence. The constituent modes of this high-frequency, short-wavelength regime are often attributed to kinetic Alfven modes which propagate at strongly oblique directions relative to the background magnetic field. However, whistler fluctuations represent an alternative hypothesis to describe short-wavelength turbulence in the solar wind and, indeed, in any collisionless, magnetized, homogeneous plasma. This presentation will describe a comparison of linear theory properties of kinetic Alfven waves and whistler fluctuations, and will apply these results to recent simulations and observations of short-wavelength turbulence in the solar wind.
Gary Peter S.
Smith Walter C.
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