A Quiet Sun Transition Region Energetically Isolated Jet: Evidence to Cool Plasma Injections Into The Hot Corona

Increasing evidence for coronal heating contributions from cooler solar atmospheric layers challenges standard solar atmospheric descriptions of bright TR emission and pervasive lower TR plasma downflows. As such, questions related to the role of dynamic transients in contributing to the total coronal energy budget are elevated. Using AIA and HMI observations in conjunction with numerical models of 3D coronal magnetic field topologies, we investigate a jet that is: erupting from a footpoint shared by heated non-potential and potential loops, energetically isolated in the TR, and occurring adjacent to a small-scale coronal filament. A non-casual relationship is established between QSTR jet dynamics and magnetic flux emergence and cancelation events, witnessed in its underlying magnetic field environment. Non-potential and potential loop demise contribute to the jet via eruptive ejections driven from cooler atmospheric layers; however, in different fashions. Small-scale flaring events from potential loop reconnection with pre-existing fields, inject both hot and cool plasma blobs to coronal heights, i.e., the adjacent QSTR jet and coronal filament. Non-potential loop dynamics preludes a medium energy microflare deposit, just below the TR at the jet's origin, that heats the jet from a cool chromospheric ballistic plasma injection. Our results are evidence to energy redistribution via chromospheric to coronal mass cycling, driven by small-scale flaring. Our results confirm speculations that cool atmospheric microflare energy deposits lead to injections of cool dense plasma to coronal heights, which here visibly shine bright as a dynamic QS transient. Finally, this work elevates arguments of non-negligible coronal heating contributions from cool atmospheric layers, in QS conditions, and increases evidence for solar wind mass feeding in the presence of dynamic QS transients.