Corotating High-Speed Streams and Interplanetary Coronal Mass Ejections: An Overview of Interplanetary Observations, Geomagnetic Effects and Energetic Particles (Invited)

Details Corotating High-Speed Streams and Interplanetary Coronal Mass Ejections: An Overview of Interplanetary Observations, Geomagnetic Effects and Energetic Particles (Invited) Corotating High-Speed Streams and Interplanetary Coronal Mass Ejections: An Overview of Interplanetary Observations, Geomagnetic Effects and Energetic Particles (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm24a..01r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM24A-01

Physics

[2102] Interplanetary Physics / Corotating Streams, [2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2114] Interplanetary Physics / Energetic Particles, [7954] Space Weather / Magnetic Storms

Scientific paper

We will review the properties of high speed solar wind streams originating in coronal holes at the Sun and interplanetary coronal mass ejections (ICMEs), the manifestations in the solar wind of coronal mass ejections at the Sun. Together these form the major solar wind drivers of magnetospheric activity. Both have different characteristics. For example, geomagnetic activity associated with high-speed streams tends to recur at the solar rotation period, extends for several days, occasionally is moderately enhanced, is most prominent at times of low solar activity and is generated by intermittent southward-turning fields associated with Alfvénic fluctuations moving way from the Sun. In contrast, activity associated with ICMEs tends to occur sporadically, can occasionally reach severe levels, is more prominent at higher activity levels, and is associated with southward field turnings in the ICME and/or the upstream sheath. More than one structure (e.g., ICME+ICME or ICME-stream) may be involved in some activity. Considering energetic particles, high-speed streams may be accompanied by ion enhancements that reach ~10 MeV/n and appear to be accelerated beyond the orbit of Earth, possibly by the forward and reverse shocks formed at the boundaries of the corotating interaction region formed at the stream leading edge. Fast ICME-driven shocks can accelerate particles as they move away from the Sun which may occasionally reach 100s of MeV. Long-term (solar cycle and longer) variations in these properties will be discussed.

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