Simulated STEREO views of the Solar Wind following the 2008 January 2 CME

The three-dimensional Hakamada-Akasofu-Fry (HAFv.1) kinematic solar wind model can be extended to predict what the Solar TErrestrial RElations Observatory (STEREO) spacecraft might expect in observing large-scale plasma clouds ejected from the Sun. In order to demonstrate this capability, the HAFv.1 model was used to simulate the observations of a coronal mass ejection (CME) on 2008 January 2 from the twin STEROE spacecraft. Projections of the Thomson-scattered white light intensity on the plane of sky, as observed by the twin STEROE, were calculated from the three dimensional simulations. These simulations of the background solar wind and the shock front compare favorably with the white light observations of plasma clouds by the STEROE A & B. It is shown that the model can be a valuable aid and guide in the identification of the shock-induced variations of the solar wind.