The kinematic properties of a dozen ‘loop-like’ coronal transients have been examined over the range 1.2–2.4 R⊙ from Sun center. Values and trends of transient geometry, including radial height, lateral width at maximum extent, distance from loop top to height of maximum width, and lateral width at a fixed height above the instrument occulting disk at 1.2 R⊙, are given. Radial and lateral speeds of expansion are tabulated, and range from 60–900 km s-1, and 10–500 km s-1, respectively. Flare-associated events are found to exhibit the highest speeds, and show little acceleration with height; on the other hand, eruptiveassociated events exhibit large accelerations (some in excess of 50 m s-2). This clear discrimination between flare and eruptive-associated events suggests that two different physical processes are present; it is suggested that flare-associated events result from an impulsive, localized input to the corona. On the other hand, accelerated, eruptive-associated events are subjected to appreciable net forces over radial heights of one solar radius (or more) above the solar limb. It is conjectured that the pressure gradient forces responsible for the generation of the solar wind may play an important role in accelerating these latter events.