The flare‐associated interplanetary (IP) shock of February 15–16, 1967, observed by Explorer 33 and Pioneer 7 is analyzed to yield an estimation of the ecliptic plane geometry of the shock surface near 1 AU. These spacecraft were separated by 23° in heliocentric longitude, and Pioneer 7 was at a distance of 1.12 AU from the sun. There was an 18.9‐hour delay between the two observations. The estimated shock normal, obtained by using a least squares shock parameter fitting procedure for the Explorer 33 data, is found to be θSE= −53° and ϕSE= 198°, which agrees within the error cone with the estimate of Hirshberg et al. (1970), obtained by using the magnetic coplanarity theorem and the Ames Research Center magnetometer data from Explorer 33. The error cone angle for the shock normal of the Explorer 33 observation was approximately 7°. This severely inclined shock normal is not typical of IP shocks. The shock normal at the Pioneer 7 position is found to be θn= −14° and ϕn= 161°, referred to the spacecraft‐sun line, by using the magnetic coplanarity theorem and Goddard Space Flight Center magnetic field data. However, the uncertainty is large (≈25° for a 1σ cone angle). Although a data gap occurred at the apparent time of passage of the disturbance at Pioneer 6, which was 85° in heliocentric longitude from Pioneer 7 and 0.83 AU from the sun, the recovered data did suggest such a passage. A consistent picture of the shock propagation is given to explain the difference in arrival times at Pioneer 6 and 7 and at Explorer 33 and the difference of the shock normals observed by Pioneer 7 and Explorer 33. The average shock speed from the sun to each spacecraft and the local speed at Explorer 33 and their relations to the position of the initiating solar flare are obtained and discussed. In the region of space between the earth and Pioneer 7 the shock surface radius of curvature in the ecliptic plane appears t