Modeling Interactions of Coronal Mass Ejections in the Lower Heliosphere

Details Modeling Interactions of Coronal Mass Ejections in the Lower Heliosphere Modeling Interactions of Coronal Mass Ejections in the Lower Heliosphere

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh33a1193l&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH33A-1193

Physics

7513 Coronal Mass Ejections, 7835 Magnetic Reconnection, 7839 Nonlinear Phenomena, 7843 Numerical Simulation Studies, 7851 Shock Waves

Scientific paper

We present a three-dimensional (3D) numerical ideal magnetohydrodynamics (MHD) model of interacting coronal mass ejections (CMEs). The simulations are based on a 3D model of a CME propagating through a bimodal solar wind characteristic of solar minimum. The model of the solar corona contains high-latitude coronal holes and a helmet streamer structure with a current sheet at the solar equator. The CMEs are driven by a 3D Gibson-Low flux rope superimposed onto the steady-state corona. Following the propagation of the first CME, the solar wind is disturbed and the second CME is launched into a less dense heliosphere. Its characteristics are different, and, notably, it shows less deceleration while propagating. Different cases corresponding to different delays between the two CME initiations have been simulated. Each simulation is performed for ten hours after the launch of the second CME. Physics based AMR has been used to capture both ejecta and associated shocks. Physical quantities are derived for each case and compared with the case of an identical CME propagating in the heliosphere without the existence of the previous CME. We have also produced synthetic white-light coronograph images of the CMEs.

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