  We consider the optical appearance under a thin accretion disk of a regular
black hole with a central de Sitter core implementing $\mathcal{O}(l^2/r^2)$
far-corrections to the Schwarzschild black hole. We use the choice $l=0.25M$,
which satisfies recently found constraints from the motion of the S2 star
around Sgr A$^*$ in this model, and which leads to thermodynamically stable
black holes. As the emission model, we suitably adapt ten samples of the
Standard Unbound emission profile for a monochromatic intensity in the disk's
frame, which have been previously employed in the literature within the context
of reproducing General Relativistic Magneto-Hydrodynamic simulations of the
accretion flow. We find the usual central brightness depression surrounded by
the bright ring cast by the disk's direct emission as well as two
non-negligible photon ring contributions. As compared to the usual
Schwarzschild solution, the relative luminosities of the latter are
significantly boosted, while the size of the former is strongly decreased. We
discuss the entanglement of the background geometry and the choice of emission
model in generating these black hole images, as well as the capability of these
modifications of Schwarzschild solution to pass present and future tests based
on their optical appearance when illuminated by an accretion disk.
