  The topology of the coronal magnetic field produces a strong impact on the
properties of the solar corona and presumably on the origin of the slow solar
wind. To advance our understanding of this impact, we revisit the concept of
so-called slip-back mapping (Titov et al. 2009) and adapt it for determining
open, closed, and disconnected flux systems that are formed in the solar corona
by magnetic reconnection during a given time interval. The developed method
allows us, in particular, to describe the magnetic flux transfer between open
and closed flux regions via so-called interchange reconnection with an
unprecedented level of details. We illustrate the application of this method to
the analysis of the global MHD evolution of the solar corona that is driven by
an idealized differential rotation of the photospheric plasma.
