HR: 1340h
AN: SH43A-1090 [Abstracts]
TI: Self-Consistent Model of the Outer Solar Wind Including Turbulence Transport
AU: * Killie, M
EM: mari.killie@ucr.edu
AF: Institute of Theoretical Astrophysics
University of Oslo, P.O.Box 1029 Blindern, Oslo, 0315
Norway
AU: * Killie, M
EM: mari.killie@ucr.edu
AF: Institute of Geophysics and Planetary Physics (IGPP), University of California, Riverside, Riverside,
CA 92521
United States
AU: Florinski, V
AF: Institute of Geophysics and Planetary Physics (IGPP), University of California, Riverside, Riverside,
CA 92521
United States
AU: Zank, G
AF: Institute of Geophysics and Planetary Physics (IGPP), University of California, Riverside, Riverside,
CA 92521
United States
AB:
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.
DE: 2149 MHD waves and turbulence
DE: 2152 Pickup ions
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting