  Pulsating binary stars are ideal targets for testing the theory of stellar
structure and evolution. Fundamental parameters can be derived to high
precision from binary modelling and provide crucial constraints for seismic
modelling. High-order gravity modes are sensitive to the conditions near the
convective core and therefore allow for a determination of parameters
describing interior physics, especially the convective-core overshooting
parameter. KIC\,10080943 is a binary system that contains two gravity- and
pressure-mode hybrid pulsators. A detailed observational study has provided
fundamental and seismic parameters for both components. We aim to find a model
that is able to predict the observed g-mode period spacings and stellar
parameters of both components of KIC 10080943. By calculating model grids with
the stellar evolution code MESA and the seismic code GYRE, we can compare
theoretical properties to the observed mean period spacing and position in the
Hertzsprung-Russell diagram. The masses of our best models are somewhat below
the values estimated from binarity, which is a consequence of the low observed
mean g-mode period spacing. We find that the amount of core overshooting and
diffusive mixing can be well constrained by the equal-age requirement for the
two stars, however, we find no significant difference for different shapes of
core overshooting. The measured rotation rates are within the limit of validity
for the first-order perturbation approximation. We can find a good fit by using
the traditional approximation for the pulsations, when taking slightly younger
models with a higher asymptotic period spacing. This is because the zonal modes
experience a slight shift due to the Coriolis force, which the first-order
perturbation approximation ignores.
