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

TL;DR

This study presents multi-instrument observations and modeling of chromospheric evaporation in a coronal loop triggered by active region transient brightenings, revealing temperature-dependent dynamics and plasma flows.

Contribution

It provides the first combined observational and simulation analysis of chromospheric evaporation linked to ARTBs in a coronal loop.

Findings

Chromospheric evaporation observed in multiple hot channels with temperature-dependent timing.

Plasma reached approximately 10 MK at footpoints and loop-top during ARTBs.

Spectroscopic data showed redshifted emission and increased line widths during evaporation.

Abstract

Using the observations recorded by Atmospheric Imaging Assembly (AIA) on-board the Solar Dynamics Observatory (SDO), the Interface Region Imaging Spectrograph (IRIS) and the Extreme-ultraviolet Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) both on-board Hinode, we present the evidence of chromospheric evaporation in a coronal loop after the occurrence of two active region transient brightenings (ARTBs) at the two footpoints. The chromospheric evaporation started nearly simultaneously in all the three hot channels of AIA such as 131~{\AA}, 94~{\AA} and 335~{\AA}, which was observed to be temperature dependent, being fastest in the highest temperature channel. The whole loop became 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 DEM measurements at the two footpoints (i.e., of two ARTBs) and the loop-top suggest that the plasma attained a maximum temperature of $\sim$10~MK at all these locations. The spectroscopic observations from IRIS revealed the presence of 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 flow at 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 shift which again preceded enhancement in the intensity. The observed results were qualitatively reproduced by 1-D hydrodynamic simulations where energy was deposited at both the footpoints of a monolithic coronal loop that mimicked the ARTBs identified in the observations.