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We study the C8.4 class solar flare SOL2016-05-14T11:34 UT usinghigh-resolution spectral imaging in the Ca ii 8542 {\AA} line obtained with theCRISP imaging spectropolarimeter on the Swedish 1-m Solar Telescope.Spectroscopic inversions of the Ca ii 8542 {\AA} line using the non-LTE codeNICOLE are used to investigate the evolution of the temperature and velocitystructure in the flare chromosphere. A comparison of the temperaturestratification in flaring and non-flaring areas reveals strong footpointheating during the flare peak in the lower atmosphere. The temperature of theflaring footpoints between continuum optical depth at 500~nm,$\mathrm{log~\tau_{500}~\approx -2.5~and~ -3.5}$ is $\mathrm{\sim5-6.5~kK}$,close to the flare peak, reducing gradually to $\mathrm{\sim5~kK}$. Thetemperature in the middle and upper chromosphere, between$\mathrm{log~\tau_{500} \approx - 3.5~and~- 5.5}$, is estimated to be$\mathrm{\sim6.5 - 20~kK}$, decreasing to pre-flare temperatures,$\mathrm{\sim5 - 10~kK}$, after approximately 15 minutes. However, thetemperature stratification of the non-flaring areas is unchanged. The invertedvelocity fields show that the flaring chromosphere is dominated by weakdownflowing condensations at the Ca ii 8542 {\AA} formation height.

Spectroscopic inversions of the Ca ii 8542 {\AA} line in a C-class solar flare