Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh31c09g&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH31C-09 INVITED
Other
2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma, 7513 Coronal Mass Ejections
Scientific paper
Coronagraph observations indicate that coronal mass ejection, CME, acceleration profiles between 2 and 30 solar radii typically fall into one of two classes. 1. CMEs with initial speeds at 2 solar radii below ~300 km/s continue to accelerate as they progress outward from the Sun, having acceleration profiles similar to that of the normal slow solar wind. 2. CMEs with initial speeds at 2 solar radii greater than ~300 km/s appear to be impulsively accelerated close to the Sun and move out to 30 solar radii with nearly constant speed. The faster CMEs in this latter class must eventually decelerate as they interact with slower ambient wind ahead and behind. The question arises: Do CMEs in these apparently distinct and different acceleration classes form distinct classes in the solar wind far from the Sun? This talk attempts to address this question. Significant bimodality exists in CME signatures in the solar wind near 1 AU, for example CMES with and without magnetic flux rope topologies, CMEs that do and do not drive shocks, CMEs with and without heavy ion enhancements, CMEs with and without mixtures of closed, open, and disconnected field lines, expanding and non-expanding CMEs, etc. However, these different bimodal classes generally are overlapping, rather than distinct from one another. Our preliminary conclusion is that these and other bimodal characteristics of CMEs in the solar wind far from the Sun do not relate directly to the two classes of CME acceleration profiles close to the Sun.
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