A. Szabo (HSTX Corp., at NASA/GSFC) , C. Farrugia (Space Science Center, U. New Hampshire, Durham, NH 03824), D. Berdichevsky (Raytheon STX Corp., at NASA/GSFC, e-mail: istp::berdi), J.-L. Bougeret (DESPA-URA CNRS 264-Obs. de Paris, 92195, Meudon, France), R. Lepping, K. Ogilvie, and M. Kaiser (NASA/GSFC, Greenbelt, MD 20771), M. Reiner (HSTX Corp., at NASA/GSFC), R. Fitzenreiter (NASA/GSFC, Greenbelt, MD 20771), and J. Steinberg (Center for Space Research, MIT, Cambridge, MA 02139)

WIND, moving toward the Earth (between 82 and 77 Earth radii), observed on Dec. 24-25, 96, an ejecta, in the form of an interplanetary magnetic cloud (IMC), from the magnetometer (MFI) and ion plasma instrument (SWE). The observational evidence is of an IMC in a slow solar wind (average velocity V=325km/s), the cloud is "isolated", i.e., is not being overtaken by faster flows, and it is not driving a shock. It has front and back magnetic holes, with the later being a current sheet. Several interplanetary type III radio bursts detected during Dec. 19 and 20, by the WIND/ WAVES instrument provided indirect signatures of the IMC in the interplanetary medium. We use the remote observations to track the progress of the disturbance from about 0.6AU to approximately 1AU. We compare the interpretation of these radio data with a determination of the cloud's age and properties at 1AU using a self-similarly expanding Lundquist solution as a model. This model also determines the underlying flux rope's orientation in space, the age of the ejecta, and its dimension in the Sun-Earth direction. We will investigate the thermodynamic boundaries of the IMC using electron and proton temperatures, provided by the WIND/SWE instrument.