Physics – Plasma Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1931m&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1931
Physics
Plasma Physics
[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7851] Space Plasma Physics / Shock Waves
Scientific paper
We numerically model coronal mass ejections (CMEs) with two distinct magnetic configurations: (1) magnetic flux rope and (2) sheared arcade with breakout field topology. Magnetic flux ropes are shown to erupt from the coronal streamer belt with initial speeds that can exceed 1000 km/s driving strong forward shocks through the bimodal (fast/slow) solar wind. The acceleration from these events tends to be impulsive followed by deceleration accompanied by an increase in mass as slower moving solar wind is accumulated by the CME. The breakout model in turn shows gradual lift off as the central arcade is sheared and then accelerates as reconnection above the arcade ensues. In more realistic cases of the breakout model, multiple reconnection points form above the central arcade and greatly reduce the acceleration of the CME. We measure the velocity and acceleration profiles for the simulated CMEs out to a distance of 30 solar radii, and find a wide range of accelerations from impulsive to gradual. We compare our model results to observed CMEs to determine if a clear relationship exists between CME acceleration and source region characteristics, which is consistent with our numerical models.
der Holst Bart van
Manchester Ward B.
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