for the spectral lines formed at higher temperatures [@2006SoPh..234...95D]. Such effects have also been seen at the footpoints of loops in quiescent active regions and are interpreted as evidence of nanoflares occurring in the corona [see e. g., @2009ApJ...694.1256T; @2017ApJ...835..244G and references therein].

![image](fig2.eps){width="98.00000%"}

![image](fig3.eps){width="95.00000%"}

As solar corona has high thermal conductivity and low plasma-$\beta$, plasma is confined within the magnetic field lines. Thus, the evolution of plasma can be well demonstrated with 1-D hydrodynamic model [see, e.g., @1987ApJ...319..465M; @2000SoPh..193...33P; @2008ApJ...683..516S]. In the current study, we present observations of two ARTBs and associated loop brightening by Atmospheric Imaging Assembly [AIA; @2012SoPh..275...17L], Interface Region Imaging Spectrograph [IRIS; @2014SoPh..289.2733D] and Extreme-ultraviolet Imaging Spectrometer [EIS; @2007SoPh..243...19C] and X-Ray Telescope [XRT; @2007SoPh..243...63G] both on-board Hinode. Based on this observation, we set up a 1-D hydrodynamic simulation to study the dynamic evolution of the coronal loop using the procedure described by [@2008ApJ...683..516S].

The rest of the paper is organized as follows. In Section \[sec:obs\], we present the observations of ARTBs and the associated loop. Physical properties of the event is described in Section \[sec:analysis\]. The hydrodynamic simulation of loop and its comparison with observational results are described in Section \[sec:model\]. Finally, we summarize and discuss 