  Solar and stellar dynamos shed small-scale and large-scale magnetic helicity
of opposite signs. However, solar wind observations and simulations have shown
that some distance above the dynamo both the small-scale and large-scale
magnetic helicities have reversed signs. With realistic simulations of the
solar corona above an active region now being available, we have access to the
magnetic field and current density along coronal loops. We show that a sign
reversal in the horizontal averages of the magnetic helicity occurs when the
local maximum of the plasma beta drops below unity and the field becomes nearly
fully force free. Hence, this reversal is expected to occur well within the
solar corona and would not directly be accessible to in-situ measurements with
the Parker Solar Probe or SolarOrbiter. We also show that the reversal is
associated with subtle changes in the relative dominance of structures with
positive and negative magnetic helicity.
