HR: 1340h
AN: SH23A-1150    [Abstracts]
TI: Turbulence Transport Throughout the Heliosphere
AU: * Breech, B
EM: breech@cis.udel.edu
AF: Dept. of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19711, United States
AU: Matthaeus, W
EM: whm@udel.edu
AF: Dept. of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19711, United States
AU: Minnie, J
EM: minnie@bartol.udel.edu
AF: Dept. of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19711, United States
AU: Bieber, J
EM: jwbieber@bartol.udel.edu
AF: Dept. of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19711, United States
AU: Oughton, S
EM: seano@waikato.ac.nz
AF: Dept. of Mathematics, University of Waikato Private Bag 3105, Hamilton, 3240, New Zealand
AU: Smith, C
EM: chuck@briaxa.sr.unh.edu
AF: Institute for the Study of Earth, Oceans and Space and Dept. of Physics, University of New Hampshire, Durham, NH 03824,
AU: Isenberg, P
EM: phil.isenberg@unh.edu
AF: Institute for the Study of Earth, Oceans and Space and Dept. of Physics, University of New Hampshire, Durham, NH 03824,
AB: 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.
DE: 7859 Transport processes
DE: 7863 Turbulence (4490)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting