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

Structured Slow Solar Wind Variability: Streamer-blob Flux Ropes and Torsional Alfv\'en Waves