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Coronal loops form the basic building blocks of the magnetically closed solarcorona yet much is still to be determined concerning their possible fine-scalestructuring and the rate of heat deposition within them. Using an improvedmulti-stranded loop model to better approximate the numerically challengingtransition region, this paper examines synthetic NASA Solar DynamicsObservatory's (SDO) Atmospheric Imaging Assembly (AIA) emission simulated inresponse to a series of prescribed spatially and temporally random, impulsiveand localised heating events across numerous sub-loop elements with a strongweighting towards the base of the structure; the nanoflare heating scenario.The total number of strands and nanoflare repetition times are variedsystematically in such a way that the total energy content remainsapproximately constant across all the cases analysed. Repeated time lagdetection during an emission time series provides a good approximation for thenanoflare repetition time for low-frequency heating. Furthermore, using acombination of AIA 171/193 and 193/211 channel ratios in combination withspectroscopic determination of the standard deviation of the loop apextemperature over several hours alongside simulations from the outlinedmulti-stranded loop model, it is demonstrated that both the imposed heatingrate and number of strands can be realised.

solar physics

Multi-Stranded Coronal Loops: Quantifying Strand Number and Heating  Frequency from Simulated Solar Dynamics Observatory (SDO) Atmospheric Imaging  Assembly (AIA) Observations