Radial Evolution of Large-Scale Solar Wind Structures (Invited)

Physics – Plasma Physics

Scientific paper

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[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle, [7800] Space Plasma Physics, [7924] Space Weather / Forecasting

Scientific paper

Stream interaction regions (SIRs) and interplanetary coronal mass ejections (ICMEs) are two types of large-scale solar wind structures. In this work we undertake a comprehensive statistical comparison of both SIRs and ICMEs at the orbits of Venus, Earth, and Jupiter, through a complete cycle of solar activity, based on systematic plasma and magnetic field criteria. The radial variation and solar-cycle variation of the occurrence rate, shock association rate, scale, velocity, maximum field intensity, maximum dynamic pressure, maximum total perpendicular pressure, and other properties of SIRs and ICMEs are all quantitatively examined. The SIR shock association rate increases from about 3% at 0.72 AU to 26% at 1 AU, and to 92% at 5.3 AU. The expected sharp stream interface occurs rarely within SIRs, from 9% at 0.72 AU to 21% at 1 AU, and to 9% at 5.3 AU. Most ICMEs are still identifiable at 5.3 AU although their structure becomes more complicated. The ICME shock rate remains about 60% from 0.72 to 5.3 AU, but the ICME expansion has significantly slowed down at 5.3 AU. SIRs become stronger and faster than ICMEs at this distance. SIRs observed by ACE and Ulysses during their latitudinal alignment are compared with ENLIL heliospheric modeling. Such comparisons demonstrate solar observations and coronal models are critical to creating a good heliospheric model. These results also suggest that the models still need a lot of improvement. In addition, observations with multiple spacecraft during Oct-Nov 2003 show that the superfast ICMEs decayed more slowly than regular ICMEs, consistent with their energetic nature.

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