  The slow solar wind is generally believed to result from the interaction of
open and closed coronal magnetic flux at streamers and pseudostreamers. We use
3-dimensional magnetohydrodynamic simulations to determine the detailed
structure and dynamics of open-closed interactions that are driven by
photospheric convective flows. The photospheric magnetic field model includes a
global dipole giving rise to a streamer together with a large parasitic
polarity region giving rise to a pseudostreamer that separates a satellite
coronal hole from the main polar hole. Our numerical domain extends out to 30
solar radii and includes an isothermal solar wind, so that the coupling between
the corona and heliosphere can be calculated rigorously. This system is driven
by imposing a large set of quasi-random surface flows that capture the driving
of coronal flux in the vicinity of streamer and pseudostreamer boundaries by
the supergranular motions. We describe the resulting structures and dynamics.
Interchange reconnection dominates the evolution at both streamer and
pseudostreamer boundaries, but the details of the resulting structures are
clearly different from one another. Additionally, we calculate in situ
signatures of the reconnection and determine the dynamic mapping from the inner
heliosphere back to the Sun for a test spacecraft orbit. We discuss the
implications of our results for interpreting observations from inner
heliospheric missions, such as Parker Solar Probe and Solar Orbiter, and for
space weather modeling of the slow solar wind.
