Geoeffectivity of Coronal Mass Ejections

Details Geoeffectivity of Coronal Mass Ejections Geoeffectivity of Coronal Mass Ejections

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ssrv..124..169k&link_type=abstract

Space Science Reviews, Volume 124, Issue 1-4, pp. 169-181

Physics

10

Coronal Mass Ejections, Magnetic Clouds, Interplanetary Shocks, Magnetic Storms, Geomagnetic Indices

Scientific paper

Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour high-latitude activity.

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