  The slow solar wind exhibits strong variability on timescales from minutes to
days, likely related to magnetic reconnection processes in the extended solar
corona. Higginson2017b presented a numerical magnetohydrodynamic simulation
which showed interchange magnetic reconnection is ubiquitous and most likely
responsible for releasing much of the slow solar wind, in particular along
topological features known as the Separatrix-Web (S-Web). Here, we continue our
analysis, focusing on two specific aspects of structured slow solar wind
variability. The first type is present in the slow solar wind found near the
heliospheric current sheet, and the second we predict should be present
everywhere S-Web slow solar wind is observed. For the first type, we examine
the evolution of three-dimensional magnetic flux ropes formed at the top of the
helmet streamer belt by reconnection in the heliospheric current sheet (HCS).
For the second, we examine the simulated remote and in situ signatures of the
large-scale torsional Alfv\'en wave (TAW) which propagates along an S-Web arc
to high latitudes. We describe the similarities and differences between the
reconnection-generated flux ropes in the HCS, which resemble the well-known
"streamer blob'' observations, and the similarly structured TAW. We discuss the
implications of our results for the complexity of the HCS and surrounding
plasma sheet, and the potential for particle acceleration, as well as the
interchange reconnection scenarios which may generate TAWs in the solar corona.
We discuss predictions from our simulation results for the dynamic slow solar
wind in the extended corona and inner heliosphere.
