  We proposed that the use of an approximate "jump condition" at the solar
transition region permits fast and accurate numerical solutions of the one
dimensional hydrodynamic equations when the corona undergoes impulsive heating.
In particular, it eliminates the need for the very short timesteps imposed by a
highly resolved numerical grid. This paper presents further examples of the
applicability of the method for cases of non-uniform heating, in particular,
nanoflare trains (uniform in space but non-uniform in time) and spatially
localised impulsive heating, including at the loop apex and base of the
transition region. In all cases the overall behaviour of the coronal density
and temperature shows good agreement with a fully resolved one dimensional
model and is significantly better than the equivalent results from a 1D code
run without using the jump condition but with the same coarse grid. A detailed
assessment of the errors introduced by the jump condition is presented showing
that the causes of discrepancy with the fully resolved code are (i) the neglect
of the terms corresponding to the rate of change of total energy in the
unresolved atmsophere, (ii) mass motions at the base of the transition region
and (iii) for some cases with footpoint heating, an over-estimation of the
radiative losses in the transition region.
