I present a study of two Herbig Ae stars that are in completely different evolutionary stages : V892 Tau and PV Cep .
Using sub arc-second interferometric observations obtained with the Combined Array for Research in Millimeter-wave Astronomy ( CARMA ) at \lambda =1.3 and 2.7 mm , I have for the first time resolved their disks .
I deduce that the 5 Myr old V892 Tau has a low dust opacity index \beta =1.1 and a disk mass of \sim 0.03 M _ { \odot } .
These values correspond to the growth of its dust into large up to centimeters size structures .
In contrast , the very young ( a few \times 10 ^ { 5 } yrs ) PV Cep has a quite high opacity index \beta =1.75 and a more massive disk 0.8 M _ { \odot } .
PV Cep has the youngest resolved disk around any Herbig Ae star .
Unlike the youngest T Tauri and Class 0 stars , which contain large and processed grains , the young Herbig Ae star , PV Cep , disk contains ISM-like unprocessed dust .
This suggests that PV Cep ’ s dust evolution is slower than T Tauri stars ’ .
I also present high spatial resolution interferometric observations of the PV Cep outflow .
The outflow inclination is consistent with the orientation of the known Herbig-Haro flow in that region , HH315 .