On the Deflection of CMEs in the Corona

Details On the Deflection of CMEs in the Corona On the Deflection of CMEs in the Corona

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh41a1639p&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH41A-1639

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7531] Solar Physics, Astrophysics, And Astronomy / Prominence Eruptions

Scientific paper

SOHO observations have revealed unambiguously that coronal mass ejections (CMEs) often do not propagate radially outwards with respect to the position of their source regions. It is commonly believed that coronal holes (CHs) play a significant role in the deflection of CMEs. For instance, it has been shown that the presence of CHs near the eruption region of a CME can explain why some interplanetary shocks arrive at Earth without a discernible ejecta behind them. Further, it has recently been proposed that the relative contribution of deflecting CMEs to the near-ecliptic ICME rate could be significant at solar minimum conditions. Despite these important implications, the deflection of CMEs itself has not received much attention. In this work, we study the deflection of CMEs in the low corona by simulations and observations. We focus especially on what role the magnetic environment of the source region as well as the size of the erupting structure has on deciding wether the CME experiences a deflection or not. Finally, we compare our simulation results to high-cadence quadrature STEREO observations of CME deflection in the low corona.

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