  Data from recent numerical simulations of the solar corona and transition
region are analysed and the magnetic field connection between the low corona
and the photosphere is found to be close to that of a potential field. The
fieldline to fieldline displacements follow a power law distribution with
typical displacements of just a few Mm. Three loops visible in emulated
Transition Region And Coronal Explorer (TRACE) filters are analysed in detail
and found to have significantly different heating rates and distributions
thereof, one of them showing a small scale heating event. The dynamical
structure is complicated even though all the loops are visible in a single
filter along most of their lengths. None of the loops are static, but are in
the process of evolving into loops with very different characteristics.
Differential Emission Measure (DEM) curves along one of the loops illustrate
that DEM curves have to be treated carefully if physical characteristics are to
be extracted.
