The kinetic forces induced by the (flare) reconnection processes make the CME propagate fastly away in all directions from the rotating Sun. For forecasting purposes, we need to know the initial speed, propagation direction and geometry of the CME as well as the uncertainties of the measurements. Furthermore, models need to be capable to simulate physical processes telling us at which distances the kinetic forces cease due to the drag by the ambient solar wind. Transit times and consequently geomagnetic effects are strongly depending on the impact speed of the CME. .