Geoeffectiveness of the interplanetary manifestations of coronal mass ejections and solar-wind stream-stream interactions

Details Geoeffectiveness of the interplanetary manifestations of coronal mass ejections and solar-wind stream-stream interactions Geoeffectiveness of the interplanetary manifestations of coronal mass ejections and solar-wind stream-stream interactions

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ap%26ss.331...91m&link_type=abstract

Astrophysics and Space Science, Volume 331, Issue 1, pp.91-104

Astronomy and Astrophysics

Astrophysics

1

Geomagnetic Storm, Coronal Mass Ejection, Stream Interaction Region, Solar Wind

Scientific paper

Coronal mass ejections and high-speed streams from the Sun, and related structures formed and evolved in interplanetary space, i.e. interplanetary manifestations of CMEs (ICMEs) and stream interaction regions (SIRs)/corotating interaction regions (CIRs), are mainly responsible for geomagnetic disturbances in the Earth's magnetic environment. However, the presence or absence of associated/finer structures of ICMEs (e.g., shock/sheath, magnetic cloud) and SIRs/CIRs (forward and reverse shocks, stream interface) might influence their geoeffectiveness as these features within large-scale structures of ICMEs and SIRs display different and varying plasma and field characteristics. In this work, we analyze the solar-wind plasma and field parameters (plasma velocity, density and pressure, magnetic field, its north-south component and electric field) together with geomagnetic activity parameters ( kp and Dst), applying the method of superposed epoch analysis. By systematically changing the time of passage of different features as epochs, e.g. discontinuities/shocks, CMEs/magnetic clouds in ICMEs and discontinuities/forward shocks in SIRs/CIRs, we study the relative geoeffectiveness of not only the large-scale structures (ICMEs/SIRs/CIRs), but of their finer features also. We critically analyze the differences in geoeffectiveness due to different structures and features, with distinct plasma/field characteristics, and we utilize these results to understand the mechanism during their interaction with geospace.

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