This period is comparable to that used in other nanoflare calculations. For example, @Reep:ApJ:2013 consider a series of nanoflares with heating timescales of 60 s. @Klimchuk:ApJ:2014 have considered even faster timescales, with 10 s duration heating events. The temperature in our calculation varies between 10$^{5}$ and 10$^{7}$ K, which are reasonable values for the solar transition region and corona. For this calculation we have set $n_{\mathrm{e}}=5 \times 10^{8}$ cm$^{-3}$, which is a typical density for the low solar corona. It is worth noting, however, that we have ignored essentially all of the hydrodynamics involved in simulating nanoflares. In reality, the heating will drive corresponding changes in the plasma density that will in turn modify the temperature. Our objective here is only to determine whether or not the neglect of EIMI can be justified.

Figure \[fig:sine\] shows that the oscillating temperature prevents the CSD from asymptoting to the CIE values. Instead, after a short transient at the beginning of the simulation, the CSD settles down into a stable oscillation around an average abundance value.

These average abundances can be significantly different depending on whether EIMI is included or neglected. Figure \[fig:sineabund\] shows the average abundances of the iron charge states for 