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Determining the preferred spatial location of the energy input to solarcoronal loops would be an important step forward towards a more completeunderstanding of the coronal heating problem. Following on from Sarkar & Walsh(2008) this paper presents a short 10e9 cm "global loop" as 125 individualstrands, where each strand is modelled independently by a one-dimensionalhydrodynamic simulation. The strands undergo small-scale episodic heating andare coupled together through the frequency distribution of the total energyinput to the loop which follows a power law distribution with index ~ 2.29. Thespatial preference of the swarm of heating events from apex to footpoint isinvestigated. From a theoretical perspective, the resulting emission measureweighted temperature profiles along these two extreme cases does demonstrate apossible observable difference. Subsequently, the simulated output is foldedthrough the TRACE instrument response functions and a re-derivation of thetemperature using different filter-ratio techniques is performed. Given themulti-thermal scenario created by this many strand loop model, a broaddifferential emission measure results; the subsequent double and triple filterratios are very similar to those obtained from observations. However, anypotential observational signature to differentiate between apex and footpointdominant heating is possibly below instrumental thresholds. The consequences ofusing a broadband instrument like TRACE and Hinode-XRT in this way arediscussed.

EUV Observational consequences of the spatial localisation of nanoflare heating within a multi-stranded atmospheric loop