Constraints on coronal heating: A large study of TR/coronal rapid brightenings using IRIS and AIA data
High-resolution observations of dynamic phenomena give insights into the properties and processes that govern the low solar atmosphere. Using the Interface Region Imaging Spectrograph (IRIS) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, analysis of the characteristics of these phenomena are possible, such as their apparent speed, temperature, and composition. Fan-shaped Jets (FSJs) are one such phenomenon. FSJs typically appear of sunspot light-bridges or over the umbral/penumbral boundary with signatures in both cool and hot channels. These jets are possibly caused by a release of tension as a result of magnetic reconnection at their foot-point. Conversely these jets may in fact be the result of a series of shock waves driving material into higher layers of the solar atmosphere. AIA and IRIS images revealed that FSJs observed at active region 12192 move across the plane of sky at speeds of 23-130 kms-1, reaching lengths of up to 26 Mm. IRIS spectroscopy results also demonstrate some blue-shift behaviour accompanied by corresponding intensity increases and line-broadening. Further details may be found at Humphries et al (2020).