| Presentation Title: | From Chromospheric Evaporation to Coronal Rain: An Investigation of the Mass and Energy Cycle of a Flare |
| Author(s): | Seray Sahin [1] & Patrick Antolin [1]
[1] Northumbria University |
Abstract:
Chromospheric evaporation (CE) and coronal rain (CR) represent two crucial phenomena encompassing the circulation of mass and energy during solar flares. While CE marks the start of the hot inflow into the flaring loop, CR marks the end, indicating the outflow in the form of cool and dense condensations. With the Interface Region Imaging Spectrograph (IRIS) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO), we examine and compare the evolution, dynamics, morphology, and energetics of the CR and CE during a C2.1 flare. The CE is directly observed in imaging and spectra in the Fe XXI line with IRIS and the Fe XVIII line of AIA, with upward average total speeds of [138+-35] km s^-1 and a temperature of [9.03+-3.28]x10^6 K. An explosive to gentle CE transition is observed, with an apparent reduction in turbulence. From quiescent to gradual flare phase, the amount and density of CR increases by a factor of ~4.4 and 6, respectively. The rain's velocity increases by 1.4, in agreement with gas pressure drag. In contrast, the clump width variation is negligible. The location and morphology of CE closely match those of the rain showers, with a similar CE sub-structure to the rain strands, reflecting fundamental scales of mass and energy transport. We obtain a CR outflow mass three times larger than the CE inflow mass, suggesting the presence of unresolved CE, perhaps at higher temperatures. The CR energy corresponds to half that of the CE. These results suggest an essential role of coronal rain in the mass-energy cycle of a flare.