We report on observations of a solar jet propagating along coronal loops taken by the Solar Dynamics Observatory ( SDO ) , the Interface Region Imaging Spectragraph ( IRIS ) and 1-m New Vacuum Solar Telescope ( NVST ) .
The ejecta of the jet consist of multi-thermal components and propagate with a speed greater than 100 km s ^ { -1 } .
Brightenings are found in the remote footpoints of the coronal loops having compact and round-shape in the H \alpha images .
The emission peak of the remote brightening in the Atmospheric Imaging Assembly ( AIA ) 94 Å passband lags 60 s behind that in the jet base .
The brightenings in the remote footpoints are believed to be consequences of heating by nonthermal electrons , MHD waves and/or conduction front generated by the magnetic reconnection processes of the jet .
The heating in the remote footpoints leads to extension of the brightening along the loops toward the jet base , which is believed to be the chromospheric evaporation .
This apparently acts as a brake on the ejecta , leading to a deceleration in the range from 1.5 to 3 km s ^ { -2 } with an error of \sim 1.0 km s ^ { -2 } when the chromospheric evaporation and the ejecta meet at locations near the loop apexes .
The dynamics of this jet allows a unique opportunity to diagnose the chromospheric evaporation from the remote footpoints , from which we deduce a velocity in the range of 330–880 km s ^ { -1 } .