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We report the smallest coronal jets ever observed in the quiet Sun withrecent high resolution observations from the High Resolution Telescopes(HRI-EUV and HRI-Ly{\alpha}) of the Extreme Ultraviolet Imager (EUI) onboardSolar Orbiter. In the HRI-EUV (174 {\AA}) images, these microjets usuallyappear 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 structuresand moving blobs can be identified in some events. A subset of these eventsalso reveal signatures in the HRI-Ly{\alpha} (H I Ly{\alpha} at 1216 {\AA})images and the extreme ultraviolet images taken by the Atmospheric ImagingAssembly onboard the Solar Dynamics Observatory. Our differential emissionmeasure analysis suggests a multi-thermal nature and an average density of~1.4x10^9 cm^(-3) for these microjets. Their thermal and kinetic energies wereestimated to be ~3.9x10^24 erg and ~2.9x10^23 erg, respectively, which are ofthe same order of the released energy predicted by the nanoflare theory. Mostevents appear to be located at the edges of network lanes and magnetic fluxconcentrations, suggesting that these coronal microjets are likely generated bymagnetic reconnection between small-scale magnetic loops and the adjacentnetwork field.

Coronal microjets in quiet-Sun regions observed with the Extreme Ultraviolet Imager onboard Solar Orbiter