Effects of the time dependence of the sun's magnetic field upon the interplanetary field in the solar wind are considered. General expressions for the interplanetary field are developed under the assumptions that the radial component of the sun's field at some reference surface r0 can be described in terms of spherical harmonics with coefficients which are functions of time represented by Fourier series and that the solar wind expands radially in a steady state flow. Some of the simplest field configurations are examined in additional detail. It is shown that the variation in the sun's field may produce elliptically polarized fluctuations in the interplanetary field; may generate field strengths in the ϑ direction, i.e., the north-south direction, that are comparable in magnitude to the spiral field; may produce Bϑ with nonzero averages over significant periods of time; and may produce systematic deviations from the nominal steady state spiral angle over such periods.