  Interferometric observations of the Sun with ALMA provide valuable diagnostic
tools for studying the small-scale dynamics of the solar atmosphere.
Estimations of the observability of the small-scale dynamics as a function of
spatial resolution for regions with different characteristic magnetic field
topology facilitate a more robust analysis of ALMA observations of the Sun. A
3D model of the solar atmosphere from the MHD code Bifrost was used to produce
high-cadence observables at mm and submm wavelengths. The synthetic observables
for receiver bands 3-10 were degraded to the angular resolution corresponding
to ALMA observations with different configurations of the interferometric array
from the most compact C1, to the more extended C7. The observability of the
small-scale dynamics was analyzed in each case. The analysis was thus also
performed for predicting the potential of future capabilities. The minimum
resolution required to study the typical small spatial scales in the solar
chromosphere depends on the characteristic properties of the target region.
Here, a range from quiet Sun to enhanced network loops is considered. Limited
spatial resolution affects the observable signatures of dynamic small-scale
brightening events in the form of reduced brightness temperature amplitudes,
potentially leaving them undetectable, and even shifts in the times at which
the peaks occur of up to tens of seconds. Conversion factors between the
observable brightness amplitude and the original amplitude in the fully
resolved simulation are provided that can be applied to observational data in
principle, but are subject to wavelength-dependent uncertainties. Predictions
of the typical appearance at the different combinations of receiver band, array
configuration, and properties of the target region are conducted.
