Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh23b1637r&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH23B-1637
Physics
2101 Coronal Mass Ejections (7513), 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2164 Solar Wind Plasma, 7513 Coronal Mass Ejections (2101)
Scientific paper
Approximately one third of all ICMEs (Interplanetary Coronal Mass Ejections) detected at one AU distance from the Sun show a smooth rotation in their magnetic field vector (often accompanied by an enhanced magnetic field strength). Theses structures are called MCs (Magnetic Clouds). Their well ordered magnetic field makes them accessible to magnetic field modelling. Assuming a specific field topology and fitting the model to the observed magnetic field data allows reconstruction of the spacecraft trajectory inside a MC. Some differences in elemental and charge-state composition between MCs and ambient solar wind are well known (Examples are: Enhanced iron charge states, enhanced O7+ to O6+ ratios, and enhanced Alpha to proton ratios). The question addressed here is whether these differences result from spacecraft trajectories through different parts of the individual MC or from a different origin of MCs as compared to the majority of ICMEs. We fitted the magnetic-field data of approximately 60 MCs observed from 2001 to 2007 by ACE (Advanced Composition Explorer) near Earth and compared the thus derived position information with solar wind composition data as measured by SWICS (Solar Wind Ion Composition Spectrometer).
Berger Laurent
Gloeckler George
Koeten M.
Rodde R.
Wimmer-Schweingruber Robert F.
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