Physics
Scientific paper
Feb 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....98.1257t&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A2, p. 1257-1276.
Physics
102
Convection, Equations Of Motion, Magnetohydrodynamic Waves, Solar Magnetic Field, Solar Wind Velocity, Correlation, Magnetic Field Configurations, Variations, Wave Equations
Scientific paper
The radial evolution of solar wind fluctuations is explained using a two-component incompressible fluctuation model. The small-scale fluctuations in the solar wind are considered as being composed of Alfven waves and convective structures. Equations of motion of the fluctuations and of the correlation functions for both Alfven waves and convective structures are derived from the one-fluid MHD equations. A combination of the correlation functions of these two components is used for a comparison with observational results. The numerical solutions are shown to describe well the basic evolution trend of the fluctuation energy, the normalized cross helicity, and the Alfven ratio. It is also shown that the basic physical process of the evolution of the convective structures is the convection of the fluctuating velocity vortex lines and the magnetic field lines by the expanding solar wind.
Marsch Eckart
Tu Chia-Ying
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