While relatively common in the outer heliosphere, forward-reverse shock pairs occur rarely in the solar wind at 1 AU. Using the combined solar wind plasma and magnetic field data from ISEE 3 for the interval from August 1978 through February 1980 we have identified several examples of such shock pairs at 1 AU. Two of these shock pair events were clearly associated with transient disturbances rather than with corotating streams. Strong bidirectional electron heat flux events, which we identify as the coronal mass ejecta (CME) driving the shocks, were detected during both of these disturbances. In the stronger of the two disturbances the reverse shock was found within the CME and was separated from the forward shock by ~0.2 AU; the pressure was nearly constant between the two shocks. On the other hand, in the weaker of the two disturbances the reverse shock had propagated entirely through the CME and trailed the forward shock by ~0.3--0.4 AU; the pressure declined substantially and monotonically between the two shocks. The overall disturbance profiles for these two events compare favorably with the results of previously published numerical simulations. On the basis of those simulations we suggest that these two events are prototypes of ''driven'' and ''blast'' distrubances, wherein the time scale of the initial velocity perturbation near the Sun is, or is not, short compared to the transit time to 1 AU. Our observations support the notion that reverse shocks in disturbances are most likely to be found near the central axes of such disturbances. ¿ American Geophysical Union 1988