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We report on observations of a solar jet propagating along coronal loopstaken by the Solar Dynamics Observatory (SDO), the Interface Region ImagingSpectragraph (IRIS) and 1-m New Vacuum Solar Telescope (NVST). The ejecta ofthe jet consist of multi-thermal components and propagate with a speed greaterthan 100 km/s. Brightenings are found in the remote footpoints of the coronalloops having compact and round-shape in the Halpha images. The emission peak ofthe remote brightening in the Atmospheric Imaging Assembly (AIA) 94 \AApassband lags 60 s behind that in the jet base. The brightenings in the remotefootpoints are believed to be consequences of heating by nonthermal electrons,MHD waves and/or conduction front generated by the magnetic reconnectionprocesses of the jet. The heating in the remote footpoints leads to extensionof the brightening along the loops toward the jet base, which is believed to bethe 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 errorof $\sim1.0$\,km s$^{-2}$ when the chromospheric evaporation and the ejectameet at locations near the loop apexes. The dynamics of this jet allows aunique opportunity to diagnose the chromospheric evaporation from the remotefootpoints, from which we deduce a velocity in the range of 330--880 km/s.

Heating at the remote footpoints as a brake on jet flows along loops in the solar atmosphere