We present the results of 1D field-aligned simulations that study the plasma response to variations in coronal heating. We treat thermal conduction by using Super Time Stepping methods (Meyer et al, MNRAS, 2012). The basic loop model consists of a hydrostatic equilibrium in thermal balance between conduction, optically thin radiation and heating. Then we include an additional release of energy, localised in the hot region near the top of the loop to increase the temperature. This drives a conduction front downwards into the transition region and facilitates chromospheric evaporation. We show that, using Super Time Stepping methods for thermal conduction, we can fully resolve the temperature and density profiles without prohibitive time-step restrictions.