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Chromospheric evaporation refers to dynamic mass motions in flare loops as aresult of rapid energy deposition in the chromosphere. These have been observedas blueshifts in X-ray and extreme-ultraviolet (EUV) spectral linescorresponding to upward motions at a few tens to a few hundreds of km/s. Pastspectroscopic observations have also revealed a dominant stationary component,in addition to the blueshifted component, in emission lines formed at hightemperatures (~10 MK). This is contradictory to evaporation models predictingpredominant blueshifts in hot lines. The recently launched Interface RegionImaging Spectrograph (IRIS) provides high resolution imaging and spectroscopicobservations that focus on the chromosphere and transition region in the UVpassband. Using the new IRIS observations, combined with coordinatedobservations from the EUV Imaging Spectrometer, we study the chromosphericevaporation process from the upper chromosphere to corona during an X1.0 flareon 2014 March 29. We find evident evaporation signatures, characterized byDoppler shifts and line broadening, at two flare ribbons separating from eachother, suggesting that chromospheric evaporation takes place in successivelyformed flaring loops throughout the flare. More importantly, we detect dominantblueshifts in the high temperature Fe XXI line (~10 MK), in agreement withtheoretical predictions. We also find that, in this flare, gentle evaporationoccurs at some locations in the rise phase of the flare, while explosiveevaporation is detected at some other locations near the peak of the flare.There is a conversion from gentle to explosive evaporation as the flareevolves.

Chromospheric Evaporation in an X1.0 Flare on 2014 March 29 Observed with IRIS and EIS