Stream Interactions and Interplanetary Coronal Mass Ejections at 0.72 AU

Details Stream Interactions and Interplanetary Coronal Mass Ejections at 0.72 AU Stream Interactions and Interplanetary Coronal Mass Ejections at 0.72 AU

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008soph..249...85j&link_type=abstract

Solar Physics, Volume 249, Issue 1, pp.85-101

Physics

12

Stream Interactions, Interplanetary Coronal Mass Ejections, Venus, Solar Wind, Inner Heliosphere, Dynamic Pressure, Flux Rope, Shock, Solar Cycle Variation, Interplanetary Magnetic Field

Scientific paper

We present comprehensive surveys of 203 stream interaction regions (SIRs) and 124 interplanetary CMEs (ICMEs) during 1979 - 1988 using Pioneer Venus Orbiter (PVO) in situ solar-wind observations at 0.72 AU and examine the solar-cycle variations of the occurrence rate, shock association rate, duration, width, maximum total perpendicular pressure ( P t), maximum dynamic pressure, maximum magnetic field intensity, and maximum velocity change of these two large-scale solar-wind structures. The medians, averages, and histogram distributions of these parameters are also reported. Furthermore, we sort ICMEs into three groups based on the temporal profiles of P t, and we investigate the variations of the fractional occurrence rate of three groups of ICMEs with solar activity. We find that the fractional occurrence rate of magnetic-cloud-like ICMEs declined with solar activity, consistent with our former 1-AU results. This study at 0.72 AU provides a point of comparison in the inner heliosphere for examining the radial evolution of SIRs and ICMEs. The width of SIRs and ICMEs increases by 0.04 and 0.1 AU, respectively, and the maximum P t decreases to about 1/3 from Venus to Earth orbit. In addition, our work establishes the statistical properties of the solar-wind conditions at 0.72 AU that control the solar-wind interaction with Venus and its atmosphere loss by related processes.

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