Origin and evolution of MHD turbulence in the solar wind

Details Origin and evolution of MHD turbulence in the solar wind Origin and evolution of MHD turbulence in the solar wind

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ncimc..13...79b&link_type=abstract

Nuovo Cimento C, Serie 1 (ISSN 0390-5551), vol. 13 C, Jan.-Feb. 1990, p. 79-87.

Computer Science

2

Magnetohydrodynamic Turbulence, Solar Wind, Solar Atmosphere, Solar Planetary Interactions, Traveling Waves

Scientific paper

The large-amplitude MHD fluctuations or turbulence observed in the solar-wind plasma and magnetic field by spacecraft such as Helios and Voyager are considered theoretically. Particular attention is given to the radial evolution of Alfvenic turbulence and possible turbulence sources and mechanisms. It is concluded that the solar atmosphere generates outward-propagating waves with a spectrum related to turbulent processes in the source region, while fluctuations with inward and outward components are produced in interplanetary space due to the development of a Kelvin-Helmholtz instability at the boundaries between flows of different speeds (i.e., where kinetic energy is dominant and stream shears are large). The rapid cascade of energy toward smaller scales and a Komolgorov spectrum then result from nonlinear interactions between modes propagating in opposite directions.

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