Computer Science – Sound
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9811483l&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A7, p. 11,483-11,500.
Computer Science
Sound
13
Compressibility Effects, Magnetohydrodynamic Stability, Plasma Oscillations, Solar Wind, Three Dimensional Models, Heliosphere, Perturbation Theory, Unsteady State
Scientific paper
Some basic properties of 3D nonsteady compressible MHD perturbations in a polytropic radial MHD wind with spherical symmetry are investigated. At a large radial distance, r, analytical solutions are derived for MHD slow- and fast-type perturbations for several rational values of the polytropic index, gamma. For the typical case of gamma less than 2, MHD fast-type perturbations always propagate relative to the wind. For the atypical case of gamma greater than 2, acoustic perturbations actually become MHD slow perturbations at large r because the sound speed is now slower than the Alfven speed, which scales as about r exp -1 at large r, and these acoustic perturbations do not propagate relative to the wind, yet the wind advects them radially outward. The increasing trends with r of the relative density and magnetic field fluctuations observed in high-speed solar winds within 0.3 to 1 AU are interpreted as a manifestation of MHD fast- and slow-type perturbations.
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