Physics
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....98.3563l&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A3, p. 3563-3584.
Physics
23
Magnetohydrodynamic Waves, Solar Wind, Wave Propagation, Heliosphere, Magnetic Field Configurations, Nonlinear Equations, Three Dimensional Motion, Wentzel-Kramer-Brillouin Method
Scientific paper
The propagation of 3D adiabatic MHD perturbations in a background MHD solar wind which is spherically symmetric is considered. For Alfven waves, previous analytical WKB, non-WKB, and asymptotic solutions at large distances as well as numerical results are extended to explicit 3D versions. For 3D MHD fast and slow perturbations, the prior perturbation scheme is generalized for a purely hydrodynamic solar wind by including a magnetic field. In general, Alfven wave flux in the solar wind is not conserved; second-order linear effects due to a 3D propagation of Alfven waves in the wind are studied. For typical solar wind parameters in the absence of dissipations, the Alfven wave flux density at the solar coronal base inferred from that observed at 1 AU is 1 to 2 orders of magnitude less than what is needed (5-8 x 10 exp 5 ergs/sq cm s) if a solar wind stream would be entirely driven and maintained by Alfven waves.
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