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Solar coronal jets are frequently occurring collimated ejections of solarplasma, originating from magnetically mixed polarity locations on the Sun ofsize scale comparable to that of a supergranule. Many, if not most, coronaljets are produced by eruptions of small-scale filaments, or minifilaments,whose magnetic field reconnects both with itself and also with surroundingcoronal field. There is evidence that minifilament eruptions are a scaled-downversion of typical filament eruptions that produce solar flares and coronalmass ejections (CMEs). Moreover, the magnetic processes building up to andtriggering minifilament eruptions, which is often flux cancelation, mightsimilarly build up and trigger the larger filaments to erupt. Thus, detailedstudy of coronal jets will inform us of the physics leading to, triggering, anddriving the larger eruptions. Additionally, such studies potentially can informus of smaller-scale coronal-jet-like features, such as jetlets and perhaps somespicules, that might work the same way as coronal jets. We propose ahigh-resolution (~0.1 pixels), high-cadence (~5 seconds) EUV-solar-imagingmission for the upcoming decades, that would be dedicated to observations offeatures of the coronal-jet size scale, and smaller-scale solar featuresproduced by similar physics. Such a mission could provide invaluable insightinto the operation of larger features such as CMEs that produce significantSpace Weather disturbances, and also smaller-scale features that could beimportant for coronal heating, solar wind acceleration, and heliosphericfeatures such as the magnetic switchbacks that are frequently observed in thesolar wind.

Future High-Resolution and High-Cadence Observations for Unraveling Small-Scale Explosive Solar Features