  For the first time, systematic studies of dwarf galaxies are being conducted
throughout the Local Volume, including Centaurus A (NGC 5128), which is the
nearest elliptical galaxy. Given Centaurus As mass (roughly ten times that of
the Milky Way), AGN activity, and recent major mergers, investigating these
dwarfs and their star formation physics is imperative. However, simulating the
faintest dwarfs in a massive galaxy like Centaurus A with sufficient resolution
in a hydrodynamic simulation is computationally expensive and currently
unfeasible. In this study, we seek to reproduce Centaurus A dwarfs using the
same star formation physics as the Milky Way. We employ the semi-analytic model
Galacticus to model dwarfs within a 600 kpc region. Utilizing astrophysical
prescriptions and parameters matching the Milky Way satellites, we explore
predictions for various properties and star formation histories (SFHs) to
investigate environmental effects. We also reproduce cumulative luminosity and
luminosity metallicity relations consistent with observations for the overall
Centaurus A satellite population, while predicting half-light radii, velocity
dispersion, and SFHs for the dwarf galaxies in Centaurus A. The agreement
between our predicted SFHs for Centaurus A dwarfs and those of the Milky Way
implies the presence of universal processes governing star formation in these
galaxies. Overall, our findings shed light on the star formation physics of
dwarf galaxies in the Centaurus A system, revealing insights into their
properties and dependence on the host environment.
