Other
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987sici.symp...31y&link_type=abstract
In Alabama Univ., Huntsville. STIP Symposium on Physical Interpretation of Solar/Interplanetary and Cometary Intervals p 31 (SEE
Other
Interplanetary Magnetic Fields, Interplanetary Medium, Intervals, Magnetic Clouds, Magnetic Fields, Solar Wind, Gravitation, Interfaces, Magnetohydrodynamic Stability, Pressure Gradients, Sun, Thermal Stresses, Translational Motion
Scientific paper
Magnetic clouds observed in interplanetary space may be regarded as extraneous bodies immersed in the magnetized medium of the solar wind. The interface between a magnetic cloud and its surrounding medium separates the internal and external magnetic fields. Polarization currents are induced in the peripheral layer to make the ambient magnetic field tangential. The motion of a magnetic cloud through the interplanetary medium may be partitioned into a translational motion of the magnetic cloud as a whole and an expansive motion of the volume relative to the axis of the magnetic cloud. The translational motion is determined by two kinds of forces, i.e., the gravitational force exerted by the Sun, and the hydromagnetic buoyancy force exerted by the surrounding medium. On the other hand, the expansive motion is determined by the pressure gradient sustaining the gross difference between the internal and external pressures and by the self-induced magnetic force that results from the interaction among the internal currents. The force resulting from the internal and external currents is a part of the hydromagnetic buoyancy force, manifested by a thermal stress caused by the inhomogeneity of the ambient magnetic pressure.
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