Coronal loops form the basic building blocks of the magnetically closed solar corona yet much is still to be determined concerning their possible fine-scale structuring and the rate of heat deposition within them. Using an improved multi-stranded loop model to better approximate the numerically challenging transition region, this article examines synthetic NASA Solar Dynamics Observatory’s (SDO) Atmospheric Imaging Assembly (AIA) emission simulated in response to a series of prescribed spatially and temporally random, impulsive and localised heating events across numerous sub-loop elements with a strong weighting towards the base of the structure: the nanoflare heating scenario. The total number of strands and nanoflare repetition times is varied systematically in such a way that the total energy content remains approximately constant across all the cases analysed. Repeated time-lag detection during an emission time series provides a good approximation for the nanoflare repetition time for low-frequency heating. Furthermore, using a combination of AIA 171/193 and 193/211 channel ratios in combination with spectroscopic determination of the standard deviation of the loop-apex temperature over several hours alongside simulations from the outlined multi-stranded loop model, it is demonstrated that both the imposed heating rate and number of strands can be realised.

日冕环构成了磁闭合日冕的基本构件，但关于它们可能的精细结构和其中的热沉积速率仍有很多待确定。本文使用改进的多链环模型来更好地近似数值上具有挑战性的过渡区域，研究合成的 NASA太阳动力学天文台(SDO)大气成像组件(AIA) 发射模拟响应一系列规定的空间和时间随机、脉冲和局部加热事件，跨越多个子回路元素，对结构的底部具有很强的权重：纳米耀斑加热场景。链的总数和纳米耀斑的重复时间以这样一种方式系统地变化，即总能量含量在所有分析的情况下保持大致恒定。在发射时间序列期间重复时滞检测为低频加热的纳米耀斑重复时间提供了一个很好的近似值。此外，