Numerical simulations of interplanetary magnetic clouds

Details Numerical simulations of interplanetary magnetic clouds Numerical simulations of interplanetary magnetic clouds

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11d..08c&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11D-08

Physics

7513 Coronal Mass Ejections, 7843 Numerical Simulation Studies

Scientific paper

We have carried out MHD simulations of the evolution of the class of CMEs known as magnetic clouds. It has been shown that such CMEs survive as flux ropes during their interaction with the solar wind. However, their shape at 1 AU depends on both their initial density and relative velocity with respect to the solar wind, and in no cases does cylindrical symmetry survive the interaction of the flux rope with the solar wind. We have investigated magentic reconnection between a CME and the solar wind, for the case of propagation in a uni-directional field and along a current sheet. Reconnection happens asymmetrically in the former case, and either on both or neither side in the latter. Finally, we have carried out a systematic study of the effective drag force operating on a CME. The drag coefficient is of order unity, but the actual motion is also influenced by the virtual mass effect.

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