Abstract
Solar flares are sudden, explosive events driven by magnetic reconnection, accompanied by energy release, and acceleration of electrons from the corona down to the chromosphere causing ambient plasma heating. It is essential to observe them during their evolutionary stages and at different atmospheric layers to understand their structure and the processes triggered.
We present a preliminary analysis of the first co-temporal observations of a flare captured by GREGOR and IRIS. The M5.7 flare occurred on May 4th, 2022, during a multi-instrument coordinated campaign using ground and space-based telescopes.
GRIS@GREGOR provided IR spectra in a sit-and-stare regime, while HiFI+@GREGOR contributed with very high temporal cadence H-alpha narrow- and broad-band images, complemented by G-band, blue continuum, TiO and Ca II H images. IRIS observed in sit-and-stare mode on a different position of the AR.
We conduct an analysis of the IR and UV data from GREGOR and IRIS to infer information about the temporal evolution of the kinetics of the flows during the first stages of the flare. We discuss the physical implications of the obtained results.