Microstructures of interplanetary coronal mass ejections during solar cycle 23

Details Microstructures of interplanetary coronal mass ejections during solar cycle 23 Microstructures of interplanetary coronal mass ejections during solar cycle 23

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh31a1159k&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH31A-1159

Physics

2109 Discontinuities, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma

Scientific paper

Magnetic cloud structure of interplanetary coronal mass ejections (ICMEs) and their surrounding regions during solar cycle 23 are investigated, using solar wind data obtained from Wind and ACE spacecraft. Selected events are 27 ICMEs that satisfy the criteria of maximum solar wind speed >600 km/s and maximum magnetic field strength >20 nT. In order to understand the geometry of ICMEs, flux rope model fitting, minimum variance analysis, and coplanarity theorem are applied for magnetic clouds, interplanetary magnetic field (IMF) discontinuities, and interplanetary shocks, respectively. Typical microstructures are categorized into three types; 1) post-shock stream with turbulent IMF, 2) deflected stream with less turbulent IMF, and 3) transition layer from sheath temperature to cloud temperature with density enhancement. From the comparison with obtained ICME geometry, it is found that these three types of microstructures can be interpreted in terms of the interaction between the ICME and background solar wind.

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