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The effect of the numerical spatial resolution in models of the solar coronaand corona / chromosphere interface is examined for impulsive heating over arange of magnitudes using one dimensional hydrodynamic simulations. It isdemonstrated that the principle effect of inadequate resolution is on thecoronal density. An underresolved loop typically has a peak density of at leasta factor of two lower than a resolved loop subject to the same heating, withlarger discrepencies in the decay phase. The temperature for under-resolvedloops is also lower indicating that lack of resolution does not "bottle up" theheat flux in the corona. Energy is conserved in the models to under 1% in allcases, indicating that this is not responsible for the low density. Instead, weargue that in under-resolved loops the heat flux "jumps across" the transitionregion to the dense chromosphere from which it is radiated rather than heatingand ablating transition region plasma. This emphasises the point that theinteraction between corona and chromosphere occurs only through the medium ofthe transition region. Implications for three dimensional magnetohydrodynamiccoronal models are discussed.

The influence of numerical resolution on coronal density in hydrodynamic models of impulsive heating