We use the observed relationship of the radial gradient of anomalous cosmic rays (ACRs), as measured in the outer heliosphere with instruments on the Voyager and Pioneer spacecraft, and the tilt of the heliospheric neutral current sheet to develop a model for the time dependence of ACRs at all radii near the helioequatorial plane. This phenomenological model reproduces the observations at 1 AU, Voyagers 1 and 2, and Pioneer 10 quite well. The model also indicates that the helioequatorial source intensity at the shock varies by a factor of 10, depending on solar magnetic polarity. The location of the solar wind termination shock during 1980-1990 is found to be 92 AU, with a best-fit of 84 AU
