[en] We present an initial set of visible light and ratio observations of a coronal transient made with the Coronagraph/Polarimeter experiment on SMM and the radioheliograph at Culgoora, Australia. An enormous loop-shaped transient observed on 1980 April 7 exhibited bright material having whiplike, nonradial motions, as well as moving and stationary radio sources. The visible and radio data are far more complete than ever before, and they allow us to establish that a moving type IV radio source was located on or very close to the fast-moving loop. Stationary sources occurred both in front of and behind the loop, in the later stages concentrating on one leg of the loop. From the combined data we are able to estimate the thermal, kinetic, and magnetic energies in the transient and, for the first time, compare them with the radiative energy of the associated flare. While further analysis is needed for detailed comparisons, it appears that the mechanical energy of the material motions exceeded the total radiative energy of the flare by a factor of 10 or more, and that the convected magnetic energy was even larger. Magnetic energy stored in the corona in the form of nonpotential fields provides a possible driving force for the transient through the expansion of these fields and conversion of the magnetic energy into mechanical energy