A three-dimensional (3-D), time-dependent, magnetohydrodynamic (MHD) model is used to simulate the interplanetary propagation of a disturbance that started in the low corona via the destabilization of a southern hemisphere helmet-streamer on April 14, 1994. A severe geomagnetic storm occurred at Earth, and a forward-reverse shock structure was detected at Ulysses (3.2 AU) at E30 degrees S60 degrees. The model is initiated at 18Rs (where Rs is the solar radius, 6.95 x 10(5) km) within the supersonic and super-Alfvenic region of the solar wind; hence no consideration is given to the disturbance's evolution from similar to 1Rs to 18Rs. We refer to the interplanetary disturbance as an interplanetary/coronal mass ejection (ICME) to indicate that it may be relevant to what has been referred to in the literature as a CME but is not related to the flux rope or magnetic cloud that has also received much attention. We find that the 3-D MHD model, with a simple pressure pulse (suggested by Yohkoh soft Xray observations), provides a satisfactory comparison with the SSC timing at Earth and the Ulysses observations.
