Stream structures in the outer heliosphere

Details Stream structures in the outer heliosphere Stream structures in the outer heliosphere

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987cath.rept.....w&link_type=abstract

Final Report Catholic Univ. of America, Washington, DC. Dept. of Mechanical Engineering.

Computer Science

Cosmic Rays, Geomagnetism, Heliosphere, Interplanetary Medium, Magnetic Disturbances, Field Strength, International Sun Earth Explorer 3, Magnetic Clouds, Shock Waves, Solar Wind, Wave Propagation

Scientific paper

Nineteen magnetic clouds are identified in the years from 1978 through 1982 and studied by the superimposed epoch method. The magnetic fluctuations, density, and temperature are enhanced ahead of the clouds preceded by shocks. Strong magnetic field intensities and low proton temperatures are observed in the clouds. A relatively large (2.5%) decrease in cosmic ray intensity is caused by the turbulent sheath behind an interplanetary shock ahead of a magnetic cloud. Only a small (0.5%) decrease in intensity is associated with the magnetic cloud itself. Magnetic clouds can produce geomagnetic activity with a decrease in the Dst index of the order of 100 gammas. The magnitude of the change in Dst index for the case when southward fields arrive first is comparable to that for the case of northward fields first, and the phase is such that geomagnetic activity is associated with the southward fields.

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