Central axial field direction in magnetic clouds and its relation to southward interplanetary magnetic field events and dependence on disappearing solar filaments

Details Central axial field direction in magnetic clouds and its relation to southward interplanetary magnetic field events and dependence on disappearing solar filaments Central axial field direction in magnetic clouds and its relation to southward interplanetary magnetic field events and dependence on disappearing solar filaments

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jgr...103.2077z&link_type=abstract

Journal of Geophysical Research, vol. 103, p. 2077

Physics

30

Solar Wind, Magnetic Clouds, Interplanetary Magnetic Fields, Solar Terrestrial Interactions, Magnetic Field Configurations, Magnetic Storms, Data Correlation, Linear Equations

Scientific paper

Extended periods of strong southward IMF B(s) are the primary cause of intense geomagnetic storms. Most of these intervals are associated with magnetic clouds in the solar wind. We define a magnetic cloud B(s) event as the interval of a southward IMF observed as a magnetic cloud passes by the Earth. For the 26 well-characterized events studied here, we find that: magnetic cloud central axial field directions are almost evenly distributed between -90- and 90-deg ecliptic latitude; the longitudinal distribution is slightly peaked around the east and west; the duration and intensity of magnetic cloud B(s) events correlate linearly with the direction of the cloud's central axial field; and cloud central axial field directions are correlated with the central axial field directions of the associated disappearing filament on the sun. These findings are useful in predicting from solar observations the duration and intensity of those magnetic cloud B(s) events that hit Earth.

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