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We numerically model the coronal mass ejection (CME) event of October 28,2003 that erupted from active region 10486 and propagated to Earth in less than20 hours causing severe geomagnetic storms. The magnetohydrodynamic (MHD) modelis formulated by first arriving at a steady state corona and solar windemploying synoptic magnetograms. We initiate two CMEs from the same activeregion, one approximately a day earlier that preconditions the solar wind forthe much faster CME on the 28th. This second CME travels through the corona ata rate of over 2500 km s$^{-1}$ driving a strong forward shock. We clearlyidentify this shock in an image produced by the Large Angle SpectrometricCoronagraph (LASCO) C3, and reproduce the shock and its appearance in syntheticwhite light images from the simulation. We find excellent agreement with boththe general morphology and the quantitative brightness of the model CME withLASCO observations. These results demonstrate that the CME shape is largelydetermined by its interaction with the ambient solar wind and may not besensitive to the initiation process. We then show how the CME would appear asobserved by wide-angle coronagraphs onboard the Solar Terrestrial RelationsObservatory (STEREO) spacecraft. We find complex time evolution of thewhite-light images as a result of the way in which the density structures passthrough the Thomson sphere. The simulation is performed with the Space WeatherModeling Framework (SWMF).

Three-Dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations