HR: 1340h
AN: SH23A-1136    [Abstracts]
TI: Density fluctuations in the solar wind : effects of nearly incompressible theory
AU: * Hunana, P
EM: peter.hunana@email.ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92507, United States
AU: Zank, G P
EM: zank@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92507, United States
AU: Shaikh, D
EM: dastgeer@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92507, United States
AB: Previously derived nearly incompressible theory with the inclusion of a simple large-scale inhomogeneous background (static and spherically symmetric) is examined by direct numerical simulations of non-stationary two dimensional turbulence. According to the theory, leading order density fluctuations satisfy a passive scalar evolution equation with additional source term induced by coupling to the large-scale inhomogeneous background. In this poster we investigate the decay rates and spectral shapes of density fluctuations together with implications for solar wind data.
DE: 2164 Solar wind plasma
DE: 7863 Turbulence (4490)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting