tokens: ; Jess et al. 2012 ; Krishna Prasad et al. 2015 , to name but a few). Wang et al. ( 2013 ) employed simulations to indicate that PDs, which are ubiquitously observed in coronal SDO /AIA observations, may be produced by small-scale impulsive heating events (e.g., nanoflares) at the loop footpoints. However, the models employed by Wang et al. ( 2013 ) utilize a more straightforward cosine-based impulsive functional form, rather than the traditional impulsive rise and gradual decay found in many small-scale flare studies. Furthermore, since Keys et al. ( 2011 ) also documented how the velocity evolution of small-amplitude flares closely matches the intensity fluctuations, the Monte Carlo–based nanoflare time series presented here could equally be employed to model intensity or velocity impulses at the base of coronal loops. These more traditional impulsive rises and exponential decays could then be fed into magnetohydrodynamic modeling codes, such as that used by Wang et al. ( 2013 ), to investigate in more detail whether nanoflares can contribute to the creation of PDs in coronal loops, fans, and plumes. Additionally, Hudson Warmuth ( 2004 ) revealed evidence to support the earlier work of Uchida ( 1968 ), whereby wave motion in coronal loops can be associated with weakly nonlinear effects originating in metric Type II bursts. Therefore, the inherent “sawtooth” shape of the nanoflare light curves may be able to help probe some of the weakest oscillating structures, especially since chromospheric and coronal fluctuations are becoming increasingly ubiquitous with continual improvements in instrument spatial and temporal resolutions (Jess et al. 2015 ; Grant et al. 2018 ; Houston et al. 2018 ). Finally, the nanoflare characterization approaches described here can also be directly applied to high time resolution observations of stellar sources (e.g., modernizing the work of Audard et al. 1999 ; Kashyap et al. 2002 ). For example, the photometric precision of high-cadence Kepler observations (Koch et al. 2010 ), or those taken through an assortment of optical filters by ULTRACAM (Dhillon et al. 2007 ) at very high cadences, would be ideal to test the nanoflare signatures on variable dwarf stars. Indeed, developing from the work of Hawley et al. ( 2014 ), Pitkin et al. ( 2014 ), Balona ( 2015 ), and Lurie et al. ( 2015 ), the initial Monte Carlo simulations could be extended to larger-amplitude values to expand the “nanoflare” coverage into more macroscopic sources that demonstrate intensity fluctuations exceeding 3 σ N . With larger-scale impulsive events being much more evident in the resulting light curves, the user would have a much better grasp of the e -folding timescales associated with the flaring activity. As a result, the occurrence rates of (quasi-)periodic activity could be much more reliably constrained, thus better revealing the energy output of such flaring events on distant stellar sources. In addition, high temporal resolution (∼0.1 s)
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