Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh51c0285m&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH51C-0285
Other
7839 Nonlinear Phenomena, 7863 Turbulence, 2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2149 Mhd Waves And Turbulence
Scientific paper
A four equation MHD turbulence model describes the radial evolution of fluctuation energy, correlation scale, temperature, and cross-helicity in a specified spherically expanding solar wind flow. This model is solved numerically along every radial direction in our simulation domain, spanning the region from 0.3 AU to 100 AU, varying inner boundary conditions and parameters to account for latitudinal structure. The model involves, as parameters, the plasma shear, wind speed, and strength of pick-up ion driving, Karman-Taylor constants, a constant that depends upon turbulence geometry, and another that specifies the ratio of kinetic to magnetic energy in the fluctuations. Magnetic variance, correlation length, cross helicity and plasma temperature are given latitudinal dependence along the inner boundary at 0.3 AU. The solar wind speed, proton number density, and temperature profiles are chosen to be consistent with observations over Ulysses' first full polar orbit [McComas et al., J. Geophys. Res., 105, 10419, 2000]. A simple model of pick-up ions is employed at present, which we plan to improve, following Isenberg et al [ApJ, 592, 564 2003]. The early indication shows that the simulation results thus obtained can be brought into good agreement with Voyager and Ulysses observations using parameters and boundary conditions that are consistent with observations. An interesting feature is that a relatively high magnetic variance is required at high latitude at inner boundary to make reasonable comparisons with observations. Heating is suppressed in the inner heliosphere and at high latitudes by the cross helicity effect, and the Alfvenicity of the turbulence almost completely vanishes by 10 AU.
Bieber John W.
Breech Ben
Burger R. A.
Isenberg Philip A.
Matthaeus William
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