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Understanding coronal mass ejection (CME) energetics and dynamics has been along-standing problem, and although previous observational estimates have beenmade, such studies have been hindered by large uncertainties in CME mass. Here,the two vantage points of the Solar Terrestrial Relations Observatory (STEREO)COR1 and COR2 coronagraphs were used to accurately estimate the mass of the2008 December 12 CME. Acceleration estimates derived from the position of theCME front in 3-D were combined with the mass estimates to calculate themagnitude of the kinetic energy and driving force at different stages of theCME evolution. The CME asymptotically approaches a mass of 3.4\pm1.0x10^15 gbeyond ~10 R_sun. The kinetic energy shows an initial rise towards6.3\pm3.7x10^29 erg at ~3 R_sun, beyond which it rises steadily to4.2\pm2.5x10^30 erg at ~18 R_sun. The dynamics are described by an early phaseof strong acceleration, dominated by a force of peak magnitude of3.4\pm2.2x10^14N at ~3 R_sun, after which a force of 3.8\pm5.4x10^13 N takesaffect between ~7-18 R_sun. These results are consistent with magnetic(Lorentz) forces acting at heliocentric distances of <7 R_sun, while solar winddrag forces dominate at larger distances (>7 R_sun).

Coronal Mass Ejection Mass, Energy, and Force Estimates Using STEREO