all important diagnostics of the chromosphere. We are motivated to do this because we want to test to what extent the MURaM simulation produces a chromosphere that resemble real observations, specifically, we are interested in whether the large spatial scales lead to long chromospheric fibrils, and how the coronal flare affects the chromosphere, despite the lack of non-thermal electrons in the model.

We compare the synthetic observations with observations taken with the Swedish 1-meter Solar Telescope [@2003SPIE.4853..341S SST;] and the Interface Region Imaging Spectrograph [@2014SoPh..289.2733D]. The paper is structured as follows: the modeling and methods are presented in Section \[sec:modeling\], an overview of the observations in Section \[sec:observation\], the results in Section \[sec:results\], and finally the discussion and conclusions are given in Section \[sec:discussion\].

Modeling {#sec:modeling}
========

Model atmosphere {#sec:model_atmosphere}
----------------

[We ran a simulation with the same setup as in [@2018NatAs.tmp..173C], but with double the spatial resolution.]{} [We use a snapshot from this simulation taken at $71$ seconds before the flare peak, which is defined as the peak of the synthetic soft X-ray flux as it would be measured by the GOES satellite.]{}

The simulation spans in the vertical direction from $-$7.5 Mm below the photosphere to 41.6 Mm 