SMEI and IPS 3-D CME Reconstructions, and What They Indicate of Heliospheric Solar Wind Acceleration

Details SMEI and IPS 3-D CME Reconstructions, and What They Indicate of Heliospheric Solar Wind Acceleration SMEI and IPS 3-D CME Reconstructions, and What They Indicate of Heliospheric Solar Wind Acceleration

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh32a..05j&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH32A-05

Astronomy and Astrophysics

Astrophysics

[2101] Interplanetary Physics / Coronal Mass Ejections, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7924] Space Weather / Forecasting

Scientific paper

The remotely-sensed measurements of coronal mass ejections (CMEs) and their interplanetary counterparts (ICMEs) from Solar Mass Ejection Imager (SMEI) white-light brightness and radio interplanetary scintillation (IPS) data can be used to provide limits on the acceleration and deceleration of transients in the inner heliosphere. As an intermediate measurement between the Sun and 1 AU, the limits provided by remote sensing are convolved with line-of-sight effects and CME/ICME `evolution' as each feature of the transient moves outward from the Sun. Here we review a few of the popular events and studies that have been presented to show how CME propagation proceeds in the inner heliosphere. Often, the apparent acceleration shown can only be provided by employing an assumption of the CME three-dimensional (3-D) shape, which often changes with solar distance and CME visibility along the line of sight. This assumption can often abrogate the original acceleration measurement. In particular we concentrate here on the analysis of two events during periods in 02-04 November 2003, and also in January 2010 showing how each event provides significantly different acceleration profiles depending on which structures are identified in each transient. Finally, we highlight the strange case of polar coronal jets (that are essentially miniature CMEs) frequently observed to move outward in the polar coronal fast wind at speeds of over three times ambient. These small solar wind transients seem to have disappeared by the time they can be observed in Ulysses in-situ data. Thus, a detailed study of these jets may provide an understanding of smaller-scale CME/ICME deceleration processes.

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