  The operation of the solar dynamo, with all of its remarkable spatio-temporal
ordering, remains an outstanding problem of modern solar physics. A number of
mechanisms that might plausibly contribute to its operation have been proposed,
but the relative role played by each remains unclear. This uncertainty stems
from continuing questions concerning the speed and structure of deep-seated
convective flows. Those flows are in-turn thought to sustain both the Sun's
turbulent EMF and the large-scale flows of differential rotation and meridional
circulation suspected of influencing the dynamo's organization and timing.
Continued progress in this area is complicated by (i) inconsistencies between
helioseismic measurements of convective and meridional flow made with different
techniques and instruments, and (ii) a lack of high-latitude data for
convection, differential rotation, and meridional flow. We suggest that the
path forward to resolving these difficulties is twofold. First, the acquisition
of long-term helioseismic and emissivity measurements obtained from a polar
vantage point is vital to complete our picture of the Sun's outer convection
zone. Second, sustained and expanded investment in theory-oriented and combined
theory/observational research initiatives will be crucial to fully exploit
these new observations and to resolve inconsistencies between existing
measurements.
