  Using EUV images and line-of-sight magnetograms from Solar Dynamics
Observatory, we examine eight emerging bipolar magnetic regions (BMRs) in
central-disk coronal holes for whether the emerging magnetic arch made any
noticeable coronal jets directly, via reconnection with ambient open field as
modeled by Yokoyama and Shibata (1995). During emergence, each BMR produced no
obvious EUV coronal jet of normal brightness, but each produced one or more
faint EUV coronal jets that are discernible in AIA 193 {\AA} images. The spires
of these jets are much fainter and usually narrower than for typical EUV jets
that have been observed to be produced by minifilament eruptions in quiet
regions and coronal holes. For each of 26 faint jets from the eight emerging
BMRs, we examine whether the faint spire was evidently made a la Yokoyama and
Shibata (1995). We find: (1) 16 of these faint spires evidently originate from
sites of converging opposite-polarity magnetic flux and show base brightenings
like those in minifilament-eruption-driven coronal jets, (2) the 10 other faint
spires maybe were made by a burst of the external-magnetic-arcade-building
reconnection of the emerging magnetic arch with the ambient open field,
reconnection directly driven by the arch's emergence, but (3) none were
unambiguously made by such emergence-driven reconnection. Thus, for these eight
emerging BMRs the observations indicate that emergence-driven external
reconnection of the emerging magnetic arch with ambient open field at most
produces a jet spire that is much fainter than in previously-reported, much
more obvious coronal jets driven by minifilament eruptions.
