  The effect of the numerical spatial resolution in models of the solar corona
and corona / chromosphere interface is examined for impulsive heating over a
range of magnitudes using one dimensional hydrodynamic simulations. It is
demonstrated that the principle effect of inadequate resolution is on the
coronal density. An underresolved loop typically has a peak density of at least
a factor of two lower than a resolved loop subject to the same heating, with
larger discrepencies in the decay phase. The temperature for under-resolved
loops is also lower indicating that lack of resolution does not "bottle up" the
heat flux in the corona. Energy is conserved in the models to under 1% in all
cases, indicating that this is not responsible for the low density. Instead, we
argue that in under-resolved loops the heat flux "jumps across" the transition
region to the dense chromosphere from which it is radiated rather than heating
and ablating transition region plasma. This emphasises the point that the
interaction between corona and chromosphere occurs only through the medium of
the transition region. Implications for three dimensional magnetohydrodynamic
coronal models are discussed.

Solar and Stellar Astrophysics