Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh61a07l&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH61A-07 INVITED
Physics
2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 2788 Storms And Substorms, 7513 Coronal Mass Ejections
Scientific paper
Various solar ejecta, halo CMEs in particular, can be effective agents in transferring significant amounts of plasma and energy from their source to Earth's magnetosphere. We will discuss CMEs as such agents, but concentrate on one class of solar ejecta, magnetic clouds, because of how relatively common they are among ejecta and also because of the effectiveness with which their quantitative properties, usually through cloud-modeling as flux ropes, can be ascertained for making comparisons to quantitative properties of their sources and sinks. We review what has been discovered in recent years about some specific aspects of magnetic clouds in their own right, as triggers for magnetic storms, and in comparison to their solar birthplace attributes, such as solar filament inclination, field polarities, and magnetic flux, in addition to the specific timing and location of the source. The common feature of the presence of heliospheric current sheet (HCS) crossings near the local observations of magnetic clouds suggests that HCS occlusion is taking place in those cases. The reason for the presence of an interplanetary shock internal to a cloud in several separate cases (at least) is not understood, but occurs a little too commonly to be ascribed solely to sources independent of those clouds. About one half of all magnetic clouds have (and usually drive) upstream interplanetary shocks, or steep pressure pulses, that in most cases possess large energy- and dynamic pressure-increases across their ramps in a stationary frame of reference. When such a sharp upstream pressure increase encounters Earth's magnetosphere it dramatically pushes it in causing a major reconfiguration of its boundary current system measured on the ground as an SSC usually some (5-10) hours before the start of the main phase of a magnetic storm. Such storms are often caused by the coupling to Earth's field of either a relatively large southward component of the IMF inside the "magnetosheath"of the shock-cloud complex or a large southward IMF inside the cloud itself. This is the result of the strong fields in these regions, especially the usually long-lasting southward Bz in the cloud per se, and/or because of the variability of the pumped up fields in the sheath. We will describe how the complexity of the shock-cloud complex can cause multiple magnetic storms, according to a recent study (private communication, C.-C. Wu).
Berdichevsky Daniel B.
Lepping Ronald P.
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