The structure of the heliospheric magnetic field, an extension of the solar
magnetic field, is influenced by dynamic processes that occur on the solar
surface and in the solar corona. Recent work has demonstrated that the int
erplay between the differential rotation of the photosphere and the nonradi
al expansion of the solar wind in the corona can lead to large-scale, syste
matic motions of the coronal magnetic field. These motions, in turn, alter
the large-scale configuration of the heliospheric field, from that of the s
tandard spiral structure. A critical analysis is presented of the processes
that drive these coronal motions and of possible effects that could limit
them. The model for the heliospheric magnetic field driven by coronal motio
ns is also contrasted with other approaches and descriptions of the coronal
and heliospheric magnetic field, e.g., potential field models for the coro
nal magnetic field. Finally, the challenges and opportunities for observing
the differences between the heliospheric magnetic field driven by coronal
motions and the standard spiral field are discussed.