In this paper we explore the nature of that 18%, or less, of all interplanetary coronal mass ejected driven shocks that have the power to accelerate solar wind/seed particle populations to energies hundreds/thousands of time the solar wind ion plasma. Interesting findings will be presented and discussed for specific observed cases when the shock passage was observed at multiple spacecraft location separated tens of degrees in heliospheric longitude and in most cases within 1 AU of the Sun. The in-situ and remote observations allow to extract results of interest not only about the shock regions associated/accelerating the SEP but also on the driver of these shock surfaces traveling very fast, in the heliosphere, outward from the Sun.