  The solar coronal heating in quiet Sun (QS) and coronal holes (CH), including
solar wind formation, are intimately tied by magnetic field dynamics. Thus, a
detailed comparative study of these regions is needed to understand the
underlying physical processes. CHs are known to have subdued intensity and
larger blueshifts in the corona. This work investigates the similarities and
differences between CHs and QS in the chromosphere using the Mg II h & k, C II
lines, and transition region using Si IV line, for regions with identical
absolute magnetic flux density (|B|). We find CHs to have subdued intensity in
all the ines, with the difference increasing with line formation height and
|B|. The chromospheric lines show excess upflows and downflows in CH, while Si
IV shows excess upflows (downflows) in CHs (QS), where the flows increase with
|B|. We further demonstrate that the upflows (downflows) in Si IV are
correlated with both upflows and downflows (only downflows) in the
chromospheric lines. CHs (QS) show larger Si IV upflows (downflows) for similar
flows in the chromosphere, suggesting a common origin to these flows. These
observations may be explained due to impulsive heating via interchange
(closed-loop) reconnection in CHs (QS), resulting in bidirectional flows at
different heights, due to differences in magnetic field topologies. Finally,
the kinked field lines from interchange reconnection may be carried away as
magnetic field rotations and observed as switchbacks. Thus, our results suggest
a unified picture of solar wind emergence, coronal heating, and near-Sun
switchback formation.

Solar and Stellar Astrophysics