CMEs, Shocks and their Radio Signatures

Details CMEs, Shocks and their Radio Signatures CMEs, Shocks and their Radio Signatures

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.87p&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Coronal mass ejections (CMEs) are large-scale transients that can be observed at a multitude of wavelengths. The dynamics of CMEs are not known in detail. In the low corona, this is partly due to the lack of imaging data and partly because other processes can mask the CME initiation and liftoff phase. Flares, filament eruptions, waves, and wave-like features often occur simultaneously with CMEs. For example, a debate exists on coronal shock waves, whether they are CME-driven or due to flares, or both. With radio emission we can trace propagating shocks, electron beams, and rising structures, and the emission source locations can reveal their origin. With radio emission we can also follow CMEs to large distances in the interplanetary space and thus obtain their full kinematics.
This overview describes some of the most recent findings from the radio signatures during CME liftoff and propagation, and discusses how well the current models on CME and shock formation agree with the observations.

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