  The \ion{Fe}{i} lines observed by the Hinode/SOT spectropolarimeter were
always seen in absorption, apart from the extreme solar limb. Here we analyse a
unique dataset capturing these lines in emission during a solar white-light
flare. We analyse the temperature stratification in the solar photosphere
during a white-light flare and compare it with the post-white-light flare
state. We used two scans of the Hinode/SOT spectropolarimeter to infer, by
means of the LTE inversion code Stokes Inversion based on Response function
(SIR), the physical properties in the solar photosphere during and after a
white-light flare. The resulting model atmospheres are compared and the changes
are related to the white-light flare. We show that the analysed white-light
flare continuum brightening is probably not caused by the temperature increase
at the formation height of the photospheric continuum. However, the photosphere
is heated by the flare approximately down to $\log \tau = -0.5$ and this
results in emission profiles of the observed \ion{Fe}{i} lines. From the
comparison with the post-white-light flare state of the atmosphere, we estimate
that the major contribution to the increase in the continuum intensity
originates in the heated chromosphere.
