  This report presents a three-dimensional (3D) numerical magnetohydrodynamics
(MHD) model of the white-light coronagraph observational phenomena known as
coronal inflows and in/out pairs. Coronal inflows in the LASCO/C2 field of view
(approximately 2-6 Rs) were thought to arise from the dynamic and intermittent
release of solar wind plasma associated with the helmet streamer belt as the
counterpart to outward-propagating streamer blobs, formed by magnetic
reconnection. This interpretation was essentially confirmed with the subsequent
identification of in/out pairs and the multispacecraft observations of their 3D
structure. The MHD simulation results show relatively narrow lanes of density
depletion form high in the corona and propagate inwards with sinuous motion
which has been characterized as `tadpole-like' in coronagraph imagery. The
height--time evolution and velocity profiles of the simulation inflows and
in/out pairs are compared to their corresponding observations and a detailed
analysis of the underlying magnetic field structure associated with the
synthetic white-light and mass density evolution is presented. Understanding
the physical origin of this structured component of the slow solar wind's
intrinsic variability could make a significant contribution to solar wind
modeling and the interpretation of remote and in-situ observations from Parker
Solar Probe and Solar Orbiter.
