Self-Consistent Model of the Outer Solar Wind Including Turbulence Transport

Details Self-Consistent Model of the Outer Solar Wind Including Turbulence Transport Self-Consistent Model of the Outer Solar Wind Including Turbulence Transport

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh43a1090k&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH43A-1090

Physics

2149 Mhd Waves And Turbulence, 2152 Pickup Ions, 2164 Solar Wind Plasma

Scientific paper

Based on models describing the transport of low-frequency MHD turbulence in the outer heliosphere, which include the effects of driving and turbulent dissipation in a simple way, one can reproduce the observed profiles for magnetic fluctuation energy and temperature out to ~ 40 AU [Zank et al. 1996; Matthaeus et al. 1999; Smith et al. 2001]. These models however do not take into account the back reaction of the heating and velocity changes, etc induced by the dissipation of fluctuations, and by pickup processes. Here, we develop a fully self-consistent model that includes conservation of mass, momentum and energy for the solar wind plasma and the pickup ions, as well as a turbulence transport model. We solve for a radial supersonic solar wind from 1 AU to 100 AU. The resulting theoretical profiles for magnetic fluctuation energy, magnetic correlation length and temperature will be compared with observations from Voyager. This consistent description of pickup ions and turbulence in the solar wind is expected to strengthen dissipation of magnetic energy as a good candidate for heating the solar wind and causing the observed non-adiabatic temperature profile.

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