  We report the smallest coronal jets ever observed in the quiet Sun with
recent high resolution observations from the High Resolution Telescopes
(HRI-EUV and HRI-Ly{\alpha}) of the Extreme Ultraviolet Imager (EUI) onboard
Solar Orbiter. In the HRI-EUV (174 {\AA}) images, these microjets usually
appear as nearly collimated structures with brightenings at their footpoints.
Their average lifetime, projected speed, width, and maximum length are 4.6 min,
62 km s^(-1), 1.0 Mm, and 7.7 Mm, respectively. Inverted-Y shaped structures
and moving blobs can be identified in some events. A subset of these events
also reveal signatures in the HRI-Ly{\alpha} (H I Ly{\alpha} at 1216 {\AA})
images and the extreme ultraviolet images taken by the Atmospheric Imaging
Assembly onboard the Solar Dynamics Observatory. Our differential emission
measure analysis suggests a multi-thermal nature and an average density of
~1.4x10^9 cm^(-3) for these microjets. Their thermal and kinetic energies were
estimated to be ~3.9x10^24 erg and ~2.9x10^23 erg, respectively, which are of
the same order of the released energy predicted by the nanoflare theory. Most
events appear to be located at the edges of network lanes and magnetic flux
concentrations, suggesting that these coronal microjets are likely generated by
magnetic reconnection between small-scale magnetic loops and the adjacent
network field.
