While fast coronal mass ejections (CMEs) have been uniquely identified as sources of transient shock-disturbances in interplanetary space, it is less understood why different kinds of plasma and magnetic field signatures are found in the individual post-shock flows. It is an open question if CMEs can produce various types of solar wind ejecta, e.g. magnetic flux ropes or flows without highly ordered internal fields. To help further clarify the consequences of fast CMEs in interplanetary space we have examined shock events measured by the Helios 1 spacecraft during the years 1979–1981 for which the associated CME has been directly observed with the coronagraph onboard the P78/1 satellite. Seventeen (68%) out of 25 shock-disturbances were followed by clearly discernible driver gas signatures, but only 7 (41%) of the driver gases were magnetic clouds.