Filamentation instability of magnetosonic waves in the solar wind environment

Details Filamentation instability of magnetosonic waves in the solar wind environment Filamentation instability of magnetosonic waves in the solar wind environment

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989jgr....9413387k&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 94, Oct. 1, 1989, p. 13387-13395.

Physics

2

Interplanetary Magnetic Fields, Magnetoacoustic Waves, Magnetohydrodynamic Stability, Propagation Modes, Solar Wind, Coupled Modes, Wave Excitation

Scientific paper

Intense magnetosonic waves, originally propagating at the right angle with the interplanetary magnetic field, can excite a purely growing mode along the interplanetary magnetic field together with two symmetric magnetosonic sidebands propagating obliquely across the magnetic field. This instability process leads to the filamentation of the magnetosonic pump waves. These two excited magnetosonic sideband modes propagate together perpendicularly across the magnetic field and, meanwhile, form a standing wave pattern along the magnetic field. The thresholds of this filamentation instability can be exceeded in the solar wind environment. It is predicted that the density fluctuations produced by the filamentation instability along the interplanetary magnetic field have wavelengths greater than, at least, a few earth radii. The polarization of the obliquely propagating magnetosonic waves excited by the filamentation instability is determined by the characteristics of the magnetosonic pump waves and the environmental plasmas.

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