Magnetic fields, plasmas, and coronal holes - The inner solar system

Details Magnetic fields, plasmas, and coronal holes - The inner solar system Magnetic fields, plasmas, and coronal holes - The inner solar system

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979ssrv...23..201b&link_type=abstract

(COSPAR, IAU, IUGG, IUPAP, and URSI, International Symposium on Solar Terrestrial Physics, Innsbruck, Austria, May 29-June 3, 19

Physics

11

Computerized Simulation, Coronal Holes, Magnetohydrodynamic Flow, Satellite Observation, Solar Magnetic Field, Solar System, Coupled Modes, Magnetohydrodynamic Waves, Solar Physics, Two Dimensional Flow

Scientific paper

Recent results concerning streams and magnetic fields in the inner solar system are reviewed. Observations have shown that MHD streams are bounded by thin shear layers within 1 AU, probably because they originate in coronal holes which have sharp boundaries. The properties of Alfvenic fluctuations in streams cannot be fully explained on the basis of the hypothesis that they are plane, transverse Alfven waves. A more complete and accurate description might be that they represent nonplanar general Alfven waves weakly coupled to a compressive mode and moving through a medium containing tangential discontinuities and other convected inhomogeneities.

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