  In recent decades our understanding of solar active regions (ARs) has
improved substantially due to observations made with better angular resolution
and wider spectral coverage. While prior AR observations have shown that these
structures were always brighter than the quiet Sun at centimeter wavelengths,
recent observations at millimeter and submillimeter wavelengths have shown ARs
with well defined dark umbrae. Given this new information, it is now necessary
to update our understanding and models of the solar atmosphere in active
regions. In this work, we present a data-constrained model of the AR solar
atmosphere, in which we use brightness temperature measurements of NOAA 12470
at three radio frequencies: 17 (NoRH), 100 and 230 GHz (ALMA). Based on our
model, which assumes that the radio emission originates from thermal free-free
and gyroresonance processes, we calculate radio brightness temperature maps
that can be compared with the observations. The magnetic field at distinct
atmospheric heights was determined in our modelling process by force-free field
extrapolation using photospheric magnetograms taken by HMI/SDO. In order to
determine the best plasma temperature and density height profiles necessary to
match the observations, the model uses a genetic algorithm that modifies a
standard quiet Sun atmospheric model. Our results show that the height of the
transition region (TR) of the modelled atmosphere varies with the type of
region being modelled: for umbrae the TR is located at 1080 +/- 20 km above the
solar surface; for penumbrae, the TR is located at 1800 +/- 50 km; and for
bright regions outside sunspots, the TR is located at 2000 +/- 100 km. With
these results, we find good agreement with the observed AR brightness
temperature maps. Our modelled AR can be used to estimate the emission at
frequencies without observational coverage.
