  Given recent observational results of interchange reconnection processes in
the solar corona and the theoretical development of the S-Web model for the
slow solar wind, we extend the analysis of the 3D MHD simulation of interchange
reconnection by Edmondson et al. (Astrophys. J. 707, 1427, 2009). Specifically,
we analyze the consequences of the dynamic streamer-belt jump that corresponds
to flux opening by interchange reconnection. Information about the magnetic
field restructuring by interchange reconnection is carried throughout the
system by Alfven waves propagating away from the reconnection region,
distributing the shear and twist imparted by the driving flows, including
shedding the injected stress-energy and accumulated magnetic helicity along
newly open fieldlines. We quantify the properties of the reconnection-generated
wave activity in the simulation. There is a localized high-frequency component
associated with the current sheet/reconnection site and an extended
low-frequency component associated with the large-scale torsional Alfven wave
generated from the interchange reconnection field restructuring. The
characteristic wavelengths of the torsional Alfven wave reflect the spatial
size of the energized bipolar flux region. Lastly, we discuss avenues of future
research by modeling these interchange reconnection-driven waves and
investigating their observational signatures.
