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We seek to quantify the relative contributions of Lorentz forces andaerodynamic drag on the propagation of solar coronal mass ejections (CMEs). Weuse Graduated Cylindrical Shell (GCS) model fits to a representative set of 38CMEs observed with the SOHO and STEREO spacecraft. We find that the Lorentzforces generally peak between 1.65 and 2.45 Rsun for all CMEs. For fast CMEs,Lorentz forces become negligible in comparison to aerodynamic drag as early as3.5--4 Rsun. For slow CMEs, however, they become negligible only by 12--50Rsun. For these slow events, our results suggest that some of the magnetic fluxmight be expended in CME expansion or heating. In other words, not all of itcontributes to directed propagation. Our results are expected to be importantin building a physical model for understanding the Sun-Earth dynamics of CMEs.

CME dynamics using STEREO & LASCO observations: the relative importance of Lorentz forces and solar wind drag