  The traditional paradigm of viscosity-dominated evolution of protoplanetary
discs has been recently challenged by magnetized disc winds. However,
distinguishing wind-driven and turbulence-driven accretion through observations
has been difficult. In this study, we present a novel approach to identifying
their separate contribution to angular momentum transport by studying the gap
and ring morphology of planet-forming discs in the ALMA continuum. We model the
gap-opening process of planets in discs with both viscous evolution and
wind-driven accretion by 2D multi-fluid hydrodynamical simulations. Our results
show that gap-opening planets in wind-driven accreting discs generate
characteristic substructures that differ from those in purely viscous discs.
Specifically, we demonstrate that discs, where wind-driven accretion dominates
the production of substructures, exhibit significant asymmetries. Based on the
diverse outputs of mock images in the ALMA continuum, we roughly divide the
planet-induced features into four regimes (moderate-viscosity dominated,
moderate-wind dominated, strong-wind dominated, inviscid). The classification
of these regimes sets up a potential method to constrain the strength of
magnetized disc wind and viscosity based on the observed gap and ring
morphology. We discuss the asymmetry feature in our mock images and its
potential manifestation in ALMA observations.
