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Solar coronal mass ejections (CMEs) are the most significant drivers ofadverse space weather at Earth, but the physics governing their propagationthrough the heliosphere is not well understood. While stereoscopic imaging ofCMEs with the Solar Terrestrial Relations Observatory (STEREO) has providedsome insight into their three-dimensional (3D) propagation, the mechanismsgoverning their evolution remain unclear due to difficulties in reconstructingtheir true 3D structure. Here we use a new elliptical tie-pointing technique toreconstruct a full CME front in 3D, enabling us to quantify its deflectedtrajectory from high latitudes along the ecliptic, and measure its increasingangular width and propagation from 2-46 solar radii (approximately 0.2 AU).Beyond 7 solar radii, we show that its motion is determined by an aerodynamicdrag in the solar wind and, using our reconstruction as input for a 3Dmagnetohydrodynamic simulation, we determine an accurate arrival time at theLagrangian L1 point near Earth.

Propagation of an Earth-directed coronal mass ejection in three dimensions