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I present a study of two Herbig Ae stars that are in completely differentevolutionary stages: V892 Tau and PV Cep. Using sub arc-second interferometricobservations obtained with the Combined Array for Research in Millimeter-waveAstronomy (CARMA) at the 1.3 and 2.7 mm wavelengths, I have for the first timeresolved their disks. I deduce that the 5 Myr old V892 Tau has a low dustopacity index $\beta$=1.1 and a disk mass of 0.03 $\msun$. These valuescorrespond to the growth of its dust into large up to centimeters sizestructures. In contrast, the very young (a few 10$^5$yrs) PV Cep has a quitehigh opacity index $\beta$ =1.75 and a more massive disk 0.8 $\msun$. PV Cephas the youngest resolved disk around any Herbig Ae star. Unlike the youngest TTauri and Class 0 stars, which contain large and processed grains, the youngHerbig Ae star, PV Cep, disk contains ISM-like unprocessed dust. This suggeststhat PV Cep's dust evolution is slower than T Tauri stars'. I also present highspatial resolution interferometric observations of the PV Cep outflow. Theoutflow inclination is consistent with the orientation of the known Herbig-Haroflow in that region, HH315.

Aperture Synthesis Imaging of V892 Tau and PV Cep: Disk Evolution