Numerical Simulation of the Interaction of Two Coronal Mass Ejections from Sun to Earth

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The Physical Processes of CME/ICME Evolution (2017, methodology): “A study by Lugaz et al. (2005a) explicitly calculated this ICME mass from both 3-”
Deriving the radial distances of wide coronal mass ejections from elongation measurements in the heliosphere - application to CME-CME interaction (2009, background): “It is expected that fast shock waves can propagate inside preceding ejections (Schmidt and Cargill, 2004; Lugaz et al., 2005) and merge with the preceding shock waves.”
THE DEFLECTION OF THE TWO INTERACTING CORONAL MASS EJECTIONS OF 2010 MAY 23–24 AS REVEALED BY COMBINED IN SITU MEASUREMENTS AND HELIOSPHERIC IMAGING (2012, background): “Similarly to what was determined in the numerical simulation of Lugaz et al. (2005), we find that, following the collision, the front of CME2 propagates with a speed comparable with, but slightly higher than the speed of the front of CME1.”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, methodology): “Numerical simulations actually show that in CME-CME interaction events, large variations in density, Alfvén speed, and magnetic field can be expected within the preceding CME (Lugaz, Manchester, and Gombosi, 2005).”