Physics
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jatp...53.1055z&link_type=abstract
(Solar-terrestrial physics; International SCOSTEP Symposium, 7th, The Hague, Netherlands, June 25-30, 1990, Selected Papers. A92
Physics
Interplanetary Magnetic Fields, Magnetic Clouds, Magnetic Storms, Solar Wind, Crossings, Ecliptic, Geomagnetism, Kp Index, Magnetic Signatures, Sudden Storm Commencements
Scientific paper
The morphology of geomagnetic storms is a sensitive function of the forcing interplanetary structures. The initial phase of a geomagnetic storm is related to the interplanetary high density structure in front of the magnetic cloud. The onset, development, and recovery of the strong main phase of the storm are controlled by the magnetic field orientation of the cloud with respect to the ecliptic plane. For a negative magnetic cloud, with the magnetic field vector first being southward, the main phase of the storm will be weakened or delayed with the decrease of both the speeds of the magnetic cloud and the ambient solar wind streams. A storm with a long delayed main phase is observed with the arrival of a positive magnetic cloud, and in the low-speed case the weak main phase can be separated from the sudden commencement by a relatively quiet period. A reduction in the recovery rate of a strong main phase may be a signature of the rear boundary crossing of the cloud. The solar wind streams behind the magnetic cloud keep affecting the slow recovery of the main phase.
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