times $t > 1000$ s, when the oscillation is stable. This reveals that neglecting EIMI overestimates the abundances of charge states below Fe$^{15+}$ and underestimates the abundance of Fe$^{15+}$ and higher charge states. These differences are up to 40%, for those ions having significant relative abundances ($y_{i}>0.01$). The size of the discrepancy depends on the timescale of the oscillation. With a shorter period of about $\tau=10$ s, the discrepancy is about 50%, while for a longer period of $\tau=60$ s, the difference is about 20%.

There are clear implications for spectroscopic diagnostics searching for nanoflares. Models that neglect EIMI will systematically underestimate the abundances of charge states Fe$^{15+}$ and above. This means that observations will see more high temperature plasma than is currently predicted. Additionally, differential emission measure spectroscopic analyses will have a higher ratio of hot to warm plasma than is predicted by current models. Thus, our results suggests that EIMI should be considered in nanoflare model calculations in order to accurately predict observed spectra.

Conclusions {#sec:conclusions}
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It has been thought that EIMI would be unimportant in many astrophysical contexts, especially in situations close to CIE. Combined with the lack of EIMI cross section data, multiple-ionization processes have 