Initially sphericla blast waves are systematically distorted in the presence of persisten latitudinal solar wind structure. This effect is to be distinguished from the nonsystematic distortion of shock waves due to varying structure in longitude, which introduces an approximately 30¿ average deflection of shock blast waves, and from initially nonspherical blast waves. The systematic latitudinal effect should be at least 25¿ at 1 AU at mid-latitudes for an equator-to-pole wind speed differential of 200 km s-1. This can be observed in the 30¿ noise level with 14 or more shock waves for statistics. The observed occurrence rate of shocks during solar maxima is sufficient to detect the effect on an out-of-the-ecliptic mission. We explore the three-dimensional geometry of corotating shock waves that form in association with long-lived solar wind streams. For a sinple but instructive case we find that the shock waves form closest to the sun in the equatorial plane. The sunward edge of the shock surface spirals around the rotational axis as one follows it away from the equatorial plane. The perpendicular distance between the rotation axis and the inner edge of the shock surface decreases with distance away from the equator but does not go to zero at any finite distance from the sun.