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Using the observations recorded by Atmospheric Imaging Assembly (AIA)on-board the Solar Dynamics Observatory (SDO), the Interface Region ImagingSpectrograph (IRIS) and the Extreme-ultraviolet Imaging Spectrometer (EIS) andX-Ray Telescope (XRT) both on-board Hinode, we present the evidence ofchromospheric evaporation in a coronal loop after the occurrence of two activeregion transient brightenings (ARTBs) at the two footpoints. The chromosphericevaporation started nearly simultaneously in all the three hot channels of AIAsuch as 131~{\AA}, 94~{\AA} and 335~{\AA}, which was observed to be temperaturedependent, being fastest in the highest temperature channel. The whole loopbecame fully brightened following the ARTBs after $\approx25$~s in 131~{\AA},$\approx 40$~s in 94~{\AA}, and $\approx 6.5$~min in 335~{\AA}. The DEMmeasurements at the two footpoints (i.e., of two ARTBs) and the loop-topsuggest that the plasma attained a maximum temperature of $\sim$10~MK at allthese locations. The spectroscopic observations from IRIS revealed the presenceof redshifted emission of $\sim$20~km~s$^{-1}$ in cooler lines like \ion{C}{2}and \ion{Si}{4} during the ARTBs that was co-temporal with the evaporation flowat the footpoint of the loop. During the ARTBs, the line width of \ion{C}{2}and \ion{Si}{4} increased nearly by a factor of two during the peak emission.Moreover, enhancement in the line width preceded that in the Doppler shiftwhich again preceded enhancement in the intensity. The observed results werequalitatively reproduced by 1-D hydrodynamic simulations where energy wasdeposited at both the footpoints of a monolithic coronal loop that mimicked theARTBs identified in the observations.

Observation and Modeling of Chromospheric Evaporation in a Coronal Loop Related to Active Region Transient Brightening