V arc interplanetary coronal mass ejections observed with the Solar Mass Ejection Imager

Details V arc interplanetary coronal mass ejections observed with the Solar Mass Ejection Imager V arc interplanetary coronal mass ejections observed with the Solar Mass Ejection Imager

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgra..11209103k&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue A9, CiteID A09103

Astronomy and Astrophysics

Astrophysics

29

Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Interplanetary Shocks, Solar Physics, Astrophysics, And Astronomy: Coronal Mass Ejections (2101), Interplanetary Physics: Instruments And Techniques

Scientific paper

Since February 2003, the Solar Mass Ejection Imager (SMEI) has been observing interplanetary coronal mass ejections (ICMEs) at solar elongation angles $\epsilon$ > 20°. The ICMEs generally appear as loops or arcs in the sky, but five show distinct outward concave shapes that we call V arcs. We expect to observe some V arcs, formed by trailing edges of ICME flux ropes or by leading ICME edges sheared by solar wind (SW) speed gradients at the heliospheric current sheet. We characterize the properties of these V arcs and compare them with average properties of all SMEI ICMEs. The typical V arc speeds argue against a slow MHD shock interpretation for their structures. We estimate the V arc solar source locations and their opening angle dynamics as tests for SW shearing. The first test contradicts but the second supports the SW shearing explanation. The implications of the small number of V arcs observed with SMEI is considered. The point P approximation used to determine the V arc locations and inferred solar source regions is critically examined in Appendix A.

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