for a particular case in astrophysics, we consider some parameters that are relevant for nanoflare heating of the solar corona.

One theory for the heating of the solar corona is that it is caused by numerous relatively small impulsive heating events known as nanoflares. These are usually thought to be caused by magnetic reconnection, although other processes could have a similar impulsive character, such as resonant wave absorption [@Klimchuk:SolPhys:2006]. Recently, there has been significant work on predicting the spectroscopic signatures of nanoflares [e.g., @Bradshaw:AA:2003; @Cargill:ApJ:2004; @Reale:ApJ:2008; @Bradshaw:ApJS:2011]. Nanoflares are predicted to heat the plasma to $\sim10^{7}$ K [@Schmelz:ApJ:2009; @Brosius:ApJ:2014]. However, simulations predict such hot plasma difficult to detect because the ionization balance needs time to adjust to the high temperature [@Bradshaw:ApJS:2011]. More detailed models have attempted to predict the temperature distribution of nanoflare heated plasma [@Bradshaw:ApJ:2012; @Reep:ApJ:2013]. All of these computations have so far neglected EIMI.

In order to estimate the possible effects of including EIMI in nanoflare models, we have performed dynamic ionization balance calculations with an oscillating temperature. Figure \[fig:sine\] shows one example of our results. Here the temperature is oscillating so that $\log T[\mathrm{K}] = 6.0 \sin(2\pi t/\tau)$, where $\tau=20$ s is the period of the oscillation. 