Propagation of the 12 May 1997 interplanetary coronal mass ejection in evolving solar wind structures

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Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, methodology): “More recent modeling efforts have been 3D and capture the structure of the solar wind, but treat CME propagation outside of the magnetosonic point (r ≈ 20RS) (Odstrcil et al. 2005).”
Deriving the radial distances of wide coronal mass ejections from elongation measurements in the heliosphere - application to CME-CME interaction (2009, unknown): “D simulation.”
The Physical Processes of CME/ICME Evolution (2017, background): “…of massively-parallel supercomputers in the late 1990’s, which have allowed the first realistic three-dimensional magnetohydrodynamic (MHD) simulations of specific CME events (e.g., Odstrcil et al. 2005; Lugaz et al. 2007; Tóth et al. 2007; Manchester et al. 2008; Taktakishvili et al. 2009).”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, methodology): “Odstrcil et al. (2005) showed that the ENLIL inner heliosphere MHD model prescribed by the empirical Wang–Sheeley–Arge (WSA) model (Arge & Pizzo 2000) was able to capture the 1 AU observations, while Cohen et al. (2007); Feng et al. (2010); van der Holst et al. (2010) used the WSA to prescribe the…”