Numerical Simulation of Interacting Magnetic Flux Ropes

Details Numerical Simulation of Interacting Magnetic Flux Ropes Numerical Simulation of Interacting Magnetic Flux Ropes

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..699o&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 699-7

Other

9

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields, Planetary Bow Shocks, Interplanetary Shocks

Scientific paper

A 212-D MHD numerical model is used to investigate the dynamic interaction between two flux ropes (clouds) in a homogeneous magnetized plasma. One cloud is set into motion while the other is initially at rest. The moving cloud generates a shock which interacts with the second cloud. Two cases with different characteristic speeds within the second cloud are presented. The shock front is significantly distorted when it propagates faster (slower) in the cloud with larger (smaller) characteristic speed. Correspondingly, the density behind the shock front becomes smaller (larger). Later, the clouds approach each other and by a momentum exchange they come to a common speed. The oppositely directed magnetic fields are pushed together, a driven magnetic reconnection takes a place, and the two flux ropes gradually coalescence into a single flux rope.

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