WE HAVE STARTED A PROGRAM TO APPLY THE NEXT GENERATION OF THE D ALESSIO MODEL TO THE INTERPRETATION OF PROTOPLANETARY DISKS CULLED FROM POPULATIONS OF DIFFERENT AGES AND EVOLUTIONARY STAGES WITH THE GOAL OF CHARACTERIZING THE CONDITIONS THAT DRIVE DISK EVOLUTION AND LEAD TO THE FORMATION OF PLANETS. OUR CODES ARE THE SUCCESSORS OF THE CODES THAT CALCULATE THE STRUCTURE AND EMISSION OF IRRADIATED ACCRETION DISKS WITH WHICH WE HAVE ALREADY MADE IMPORTANT DISCOVERIES SUCH AS THE IDENTIFICATION OF DISKS WITH GAPS AND THE FIRST FINDING OF WATER ICE. THE NEW MODELS CALCULATE THE STRUCTURE OF THE DUST AND OF THE GAS SEPARATELY BUT SELF-CONSISTENTLY AND INCLUDE SEVERAL ASPECTS THAT HAVE NOT BEEN FULLY TAKEN INTO ACCOUNT BEFORE: (A) VISCOUS DISSIPATION AS A HEATING AGENT OF THE GAS; (B) SOLUTION OF THE DISK STRUCTURE EQUATIONS TO GET SELF-CONSISTENT HYDROSTATIC STRUCTURES OF GAS AND DUST; (C) GAS ABSORPTION IN THE TRANSPORT OF HIGH ENERGY RADIATION IN ADDITION TO DUST; (D) DUST PROPERTIES (MINERALOGY SIZE DISTRIBUTIONS SUBLIMATION TEMPERATURES CONSISTENT WITH THE CHEMISTRY VERTICAL AND RADIAL DISTRIBUTION) INFERRED FROM THE MODELING OF THE SED AND/OR RESULTS OF NUMERICAL SIMULATIONS; (E) FLEXIBILITY IN THE CODE TO ALLOW FOR SURFACE DENSITY DISTRIBUTIONS OF GAS AND OF DUST INCLUDING RESULTS FROM NUMERICAL MODELS OF TURBULENT MRI-DRIVEN DISKS WITH RADIAL DRIFT AND TRAPPING OF DUST. HERE WE PROPOSE TO MODEL THE DISKS OF STARS STILL EMBEDDED IN THEIR INFALLING ENVELOPES AND TO INCLUDE SELF-CONSISTENTLY THE INTERACTION OF THE DISK AND THE ENVELOPE. WE WILL CALCULATE THE STRUCTURE OF THE DISK AROUND HL TAU AND IN PARTICULAR THE LOCATION OF THE CONDENSATION FRONTS OF VOLATILES FOR COMPARISON WITH OBSERVATIONS. OUR MODELING WILL PROVIDE MUCH INSIGHT INTO THE NATURE OF THE RADIAL SUBSTRUCTURE IN PROTOPLANETARY DISKS AND THE BEST REPRESENTATION OF THE EARLY SOLAR NEBULA.