Turbulence Transport Throughout the Heliosphere

Details Turbulence Transport Throughout the Heliosphere Turbulence Transport Throughout the Heliosphere

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh23a1150b&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-1150

Statistics

Computation

7859 Transport Processes, 7863 Turbulence (4490)

Scientific paper

We employ a turbulence transport model to compute distributions of turbulence throughout the heliosphere. The model determines the radial dependence of three (coupled) quantities that characterize interplanetary turbulence - the energy per unit mass, the cross helicity or Alfvénicity, and a similarity length scale. A fourth integrated quantity, the plasma (proton) temperature, is modified by heat deposition due to a von Kármán type turbulence dissipation that represents decay of turbulence due to cascade to small scales. The model includes effects of two types of driving; 1) a simple model of stream shear, which is more active in the inner heliosphere; and 2) wave energy injection due to pickup protons of interstellar origin, which is more active in the outer heliosphere. Parameters for the model have been tuned using observation data from Voyager and Ulysses. We analyze the constraining observations to provide boundary conditions and parameters that vary with heliocentric latitude, with some extrapolations. The fully assembled model permits the computation of the distribution of turbulence throughout the entire heliosphere, and we present solutions for several appropriate parameter sets.

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