Several post-AGB binaries appear to be surrounded by disks of dust and gas. These disks are formed from the matter expelled from the evolved star at the end of the AGB phase that gravitationally interacted with the companion. The disks display a Keplerian rotation profile and share several common features with protoplanetary disks around young stars despite a different formation scenario. We will present the near-infrared interferometric imaging observations of the circumbinary disk around the post-AGB binary system IRAS08544-4431. A classical radiative transfer model of a protoplanetary disk in hydrostatic equilibrium is able to reproduce both the SED and the interferometric observations. As in protoplanetary disks, the inner disk rim seems to be ruled by dust sublimation physics. However, we find non-axisymmetric structures in the disk that likely originate from the disk/binary interactions. Studying these disks more deeply could reveal that they can be a promising place for second-generation planet formation.