RECENT HIGH ANGULAR RESOLUTION OBSERVATIONS (E.G. ALMA VLT) OF PROTOPLANETARY DISKS HAVE BEGUN TO REVEAL COMPLICATED STRUCTURE (E.G. SPIRAL ARMS GAPS RINGS ETC.). IN PRINCIPLE SUCH OBSERVATIONS CAN PROVIDE CONSTRAINTS ON DISK DYNAMICS AND FOR THE FIRST TIME REVEAL THE PHYSICAL PROCESSES WHICH CONTROL THE PLANET FORMATION PROCESS. HOWEVER THIS REQUIRES REALISTIC THEORETICAL MODELS OF DISK DYNAMICS INCLUDING A PROPER TREATMENT OF MHD EFFECTS DUST GROWTH SETTLING AND FEEDBACK AS WELL AS ACCURATE RADIATIVE TRANSFER CALCULATIONS THAT CAN GENERATE SYNTHETIC IMAGES FOR COMPARISON TO DATA. THE GOAL OF THIS PROJECT IS TO COMPUTE SUCH MODELS. WE WILL CALCULATE THE MOST REALISTIC GLOBAL NUMERICAL MODELS OF PROTOPLANETARY DISKS AND DISK-PLANET INTERACTION TO DATE COMPUTE SYNTHETIC IMAGES OF THE MODELS BASED ON A SELF-CONSISTENT TREATMENT OF THE DUST DYNAMICS IN THE DISK AND COMPARE THESE MODELS TO INTERPRET EXISTING DATA AND TO PREDICT FUTURE OBSERVATIONS. IN PARTICULAR WE WILL COMPARE OUR MODELS WITH OBSERVATIONS FROM EXISTING NASA SPACE MISSIONS (E.G. SPITZER HERSCHEL) AND GROUND BASED TELESCOPES (E.G. ALMA EVLA VLT SUBARU GEMINI) AND WE WILL MAKE PREDICTIONS FOR FUTURE OBSERVATIONS. OVER YEARS OUR TEAM HAS BEEN BUILDING TOOLS TO ACHIEVE SUCH GOALS. WE HAVE STUDIED NON-IDEAL MHD EFFECTS ON DISK TURBULENCE DUST PARTICLE DYNAMICS IN GASEOUS DISKS PLANET-DISK INTERACTION AND OTHER ASTROPHYSICAL DISK RELATED PROBLEMS. NOW ADOPTING NOVEL NUMERICAL TECHNIQUES IN OUR NEWLY DEVELOPED 3-D MAGNETOHYDRODYNAMIC (MHD) CODE ATHENA++ WE CAN FINALLY PUT ALL THESE PIECES TOGETHER AND CONSTRUCT FIRST-PRINCIPLE GLOBAL SIMULATIONS TO BE DIRECTLY COMPARED WITH OBSERVATIONS. WE PLAN TO USE THIS NEW CODE TO (1) STUDY HOW PROTOPLANETARY DISKS ACCRETE BY CARRYING OUT GLOBAL 3-D MHD SIMULATIONS INCLUDING ALL IMPORTANT NON-IDEAL MHD EFFECTS. (2) INCLUDE DUST PARTICLES AND YOUNG PLANETS IN OUR SIMULATIONS TO STUDY DUST DYNAMICS PLANETESIMAL FORMATION AND THE OBSERVATIONAL SIGNATURES OF YOUNG PLANETS IN PROTOPLANETARY DISKS. SINCE MOST DISK EMISSION COMES FROM DUST THIS STEP IS ESSENTIAL FOR CONNECTING SIMULATIONS WITH OBSERVATIONS. (3) POST PROCESS OUR GLOBAL 3-D SIMULATIONS WITH 3-D MONTE CARLO RADIATIVE TRANSFER CODES TO GENERATE OBSERVATIONAL SIGNATURES OF DISK TURBULENCE AND YOUNG PLANETS IN DISKS. COMPARISONS WITH CURRENT OBSERVATIONS AND PREDICTIONS FOR FUTURE OBSERVATIONS WILL BE MADE. THESE FIRST-PRINCIPLE CALCULATIONS (INCLUDING MHD EFFECTS DUST-GAS DYNAMICS AND RADIATIVE TRANSFER) WILL ADDRESS FUNDAMENTAL QUESTIONS ON PROTOPLANETARY DISKS AND ALLOW US TO STUDY PLANET FORMATION PROCESSES IN DETAIL. THE PREDICTIONS FROM THESE SIMULATIONS WILL NOT ONLY BE COMPARED WITH OBSERVATIONS (E.G. ALMA) DIRECTLY BUT ALSO SERVE AS A FOUNDATION FOR UNDERSTANDING PLANET FORMATION AND EXOPLANET PROPERTIES FOR FUTURE SPACE MISSIONS (E.G. JWST WFIRST TESS).