2010A&A...514A..94L

Stellar flares affect all atmospheric layers from the photosphere over chromosphere and transition region up into the corona. Simultaneous observations in different spectral bands allow to obtain a comprehensive picture of the environmental conditions and the physical processes going on during different phases of the flare. We investigate the properties of the coronal plasma during a giant flare on the active M dwarf CN Leo observed simultaneously with the UVES spectrograph at the VLT and emXMM-Newton. From the X-ray data, we analyze the temporal evolution of the coronal temperature and emission measure, and investigate variations in electron density and coronal abundances during the flare. Optical Fexiii line emission traces the cooler quiescent corona. Although of rather short duration (exponential decay time τ_LC<5min), the X-ray flux at flare peak exceeds the quiescent level by a factor of ≃100. The electron density averaged over the whole flare is greater than 5x10¹¹cm^–3. The flare plasma shows an enhancement of iron by a factor of ≃2 during the rise and peak phase of the flare. We derive a size of <9000km for the flaring structure from the evolution of the the emitting plasma during flare rise, peak, and decay. The characteristics of the flare plasma suggest that the flare originates from a compact arcade instead of a single loop. The combined results from X-ray and optical data further confine the plasma properties and the geometry of the flaring structure in different atmospheric layers.