  We model a coronal loop as a three-dimensional magnetic cylinder in a
realistic solar atmosphere that extends from the chromosphere to the corona.
Kink oscillations, believed ubiquitous in the solar corona, are launched in the
loop. Heating is expected due to the dissipation of wave energy at small
structures that develop from the Kelvin-Helmholtz instability induced by kink
oscillations. Increases in temperature and internal energy can be observed in
the coronal counterpart of the driven loop. With the presence of thermal
conduction, chromospheric evaporation can also be seen. Although the volume
averaged temperature and density changes seem slight ($\sim4\%$ relative to a
non-driven loop), the enthalpy flow from the lower atmosphere redistributes the
density and temperature in the vertical direction, thus enhancing the
dissipation of wave energy in the corona. The efficient heating in the coronal
counterpart of the loop can complement the thermal conductive losses shown in
the current model and thus maintain the internal energy in the corona.
