A strong shock that would propagate spherically from the Sun were the solar wind homogeneous instead warps as it refracts and shears through inhomogeneities in solar wind density and velocity. The inhomogeneities can be disordered or ordered by quasi-permanent coronal structures such as coronal holes and the coronal streamer belt. Distortions caused by interacting solar wind streams from coronal holes have been studied. Where colliding streams build density ridges, the shock slows, producing marked localized dimples (concave outward) in the shock front. Here we note that a similar dimple results from the high-density, low-velocity inhomogeneity that distinguishes the coronal streamer belt. That is, a concave outward dimple characterizes the part of the shock that crosses the belt. First, to illustrate this effect, we apply the linearized hydrodynamic model that reveals shock dimples at density ridges of colliding streams. Then, to test the effect, we present normals of the eight shocks we could independently assess to be within the expected range of influence of the belt. Six of the eight shocks showed the predicted distortion. The null hypothesis would give the same result in 1 out of 14 tries. Finally, we note that the dimple shape induces a postshock confluence in the center of the belt of material pushed centerward from the top and bottom of the belt. We suggest this confluence of material might drive field line reconnection at the heliospheric current sheet in the center of the belt, as MHD simulations have observed. ¿ American Geophysical Union 1992