  The solar wind is connected to the Sun's atmosphere by flux tubes that are
rooted in an ever-changing pattern of positive and negative magnetic polarities
on the surface. Observations indicate that the magnetic field is filamentary
and intermittent across a wide range of spatial scales. However, we do not know
to what extent the complex flux tube topology seen near the Sun survives as the
wind expands into interplanetary space. In order to study the possible
long-distance connections between the corona and the heliosphere, we developed
new models of turbulence-driven solar wind acceleration along empirically
constrained field lines. We used a potential-field model of the Quiet Sun to
trace field lines into the ecliptic plane with unprecedented spatial resolution
at their footpoints. For each flux tube, a one-dimensional model was created
with an existing wave/turbulence code that solves equations of mass, momentum,
and energy conservation from the photosphere to 4 AU. To take account of
stream-stream interactions between flux tubes, we used those models as inner
boundary conditions for a time-steady MHD description of radial and
longitudinal structure in the ecliptic. Corotating stream interactions smear
out much of the smallest-scale variability, making it difficult to see how
individual flux tubes on granular or supergranular scales can survive out to 1
AU. However, our models help clarify the level of "background" variability with
which waves and turbulent eddies should be expected to interact. Also, the
modeled fluctuations in magnetic field magnitude were seen to match measured
power spectra quite well.
