  Plasma outflows from the edges of active regions have been suggested as a
possible source of the slow solar wind. Spectroscopic measurements show that
these outflows have an enhanced elemental composition, which is a distinct
signature of the slow wind. Current spectroscopic observations, however, do not
have sufficient spatial resolution to distinguish what structures are being
measured or to determine the driver of the outflows. The High-resolution
Coronal Imager (Hi-C) flew on a sounding rocket in May, 2018, and observed
areas of active region outflow at the highest spatial resolution ever achieved
(250 km). Here we use the Hi-C data to disentangle the outflow composition
signatures observed with the Hinode satellite during the flight. We show that
there are two components to the outflow emission: a substantial contribution
from expanded plasma that appears to have been expelled from closed loops in
the active region core, and a second contribution from dynamic activity in
active region plage, with a composition signature that reflects solar
photospheric abundances. The two competing drivers of the outflows may explain
the variable composition of the slow solar wind.
