Using global MHD simulations to interpret in situ observations of CMEs

Details Using global MHD simulations to interpret in situ observations of CMEs Using global MHD simulations to interpret in situ observations of CMEs

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh42a07r&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH42A-07

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 7509 Corona, 7513 Coronal Mass Ejections

Scientific paper

In this study, we combine two MHD models to simulate the initiation, propagation, and dynamic evolution of flux-rope-like CMEs through the corona and out to 1 AU. The coronal model encompasses the region of the solar corona from 1 Rs to 20 Rs, while the heliospheric model encompasses 20 Rs to 1 AU. The CME is initiated in the corona and propagates smoothly across the outer boundary of the coronal solution and through the inner boundary of the heliospheric solution. The model solutions show a rich complexity, which, given the relative simplicity and idealization of the input conditions, bear a strong resemblance to many observed events, and we use the simulation results to infer the global structure of some of these observations. In particular, we highlight an event that was observed by both Ulysses and ACE in February/March, 1999. At this time, Ulysses was located at ~ 5 AU and S 22 ° heliographic latitude; thus the two spacecraft were separated significantly both in heliocentric distance and latitude. We also use these simulations to separate dynamical effects from force-free models of flux ropes in the solar wind.

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