  We present a new methodology -- the Keplerian Optical Dynamics Analysis
(KODA) -- for analyzing the dynamics of dense, cool material in the solar
corona. The technique involves adaptive spatiotemporal tracking of propagating
intensity gradients and their characterization in terms of time-evolving
Keplerian areas swept out by the position vectors of moving plasma blobs.
Whereas gravity induces purely ballistic motions consistent with Kepler's
second law, non-central forces such as the Lorentz force introduce non-zero
torques resulting in more complex motions. KODA algorithms enable direct
evaluation of the line-of-sight component of the net torque density from the
image-plane projection of the areal acceleration. The method is applied to the
prominence eruption of 2011 June 7, observed by the Solar Dynamics
Observatory's Atmospheric Imaging Assembly. Results obtained include
quantitative estimates of the magnetic forces, field intensities, and blob
masses and energies across a vast region impacted by the post-reconnection
redistribution of the prominence material. The magnetic pressure and energy are
strongly dominant during the early, rising phase of the eruption, while the
dynamic pressure and kinetic energy become significant contributors during the
subsequent falling phases. Measured intensive properties of the prominence
blobs are consistent with those of typical active-region prominences; measured
extensive properties are compared with those of the whole pre-eruption
prominence and the post-eruption coronal mass ejection of 2011 June 7, all
derived by other investigators and techniques. We argue that KODA provides
valuable information on characteristics of erupting prominences that are not
readily available via alternative means, thereby shedding new light on their
environment and evolution.
