UNDERSTANDING THE PHYSICS OF ACCRETION FLOWS IN CIRCUMSTELLAR DISK PROVIDES THE FOUNDATION TO ANY THEORY OF PLANET FORMATION. THE LAST FEW YEARS HAVE WITNESSED DRAMATIC A REVISION IN THE FUNDAMENTAL FLUID DYNAMICS OF PROTOPLANETARY ACCRETION DISKS. THERE IS GROWING EVIDENCE THAT THE KEY TO ANSWERING SOME OF THE MOST PRESSING QUESTIONS SUCH AS THE ORIGIN OF DISK TURBULENCE MASS TRANSPORT AND PLANETESIMAL FORMATION MAY LIE WITHIN AND INTIMATELY LINKED TO PURELY HYDRODYNAMICAL PROCESSES IN PROTOPLANETARY DISKS. RECENT STUDIES INCLUDING THOSE FROM THE PROPOSAL TEAM HAVE DISCOVERED AND HIGHLIGHTED THE SIGNIFICANCE OF SEVERAL NEW HYDRODYNAMICAL INSTABILITIES IN THE PLANET-FORMING REGIONS OF THESE DISKS. THESE INCLUDE BUT NOT LIMITED TO: THE VERTICAL SHEAR INSTABILITY ACTIVE BETWEEN 10 TO 100 AU; THE ZOMBIE VORTEX INSTABILITY OPERATING IN REGIONS INTERIOR TO ABOUT 1AU; AND THE CONVECTIVE OVER-STABILITY AT INTERMEDIATE RADII. SECONDARY ROSSBY-WAVE AND ELLIPTIC INSTABILITIES MAY ALSO BE TRIGGERED FEEDING OFF THE STRUCTURES THAT EMERGE FROM THE ABOVE PRIMARY INSTABILITIES. THE RESULT OF THESE HYDRODYNAMIC PROCESSES RANGE FROM SMALL-SCALE TURBULENCE THAT TRANSPORTS ANGULAR MOMENTUM TO LARGE-SCALE VORTICES THAT CONCENTRATE DUST PARTICLES AND ENHANCE PLANETESIMAL FORMATION. HYDRODYNAMIC PROCESSES PERTAIN TO A WIDE RANGE OF DISK CONDITIONS MEANING THAT AT LEAST ONE OF THESE PROCESSES ARE ACTIVE AT ANY GIVEN DISK LOCATION AND EVOLUTIONARY EPOCH. THIS REMAINS TRUE EVEN AFTER PLANET FORMATION WHICH AFFECTS THEIR SUBSEQUENT ORBITAL EVOLUTION. HYDRODYNAMICAL PROCESSES ALSO HAVE DIRECT OBSERVABLE CONSEQUENCES. FOR EXAMPLE VORTICES HAVE BEING INVOKED TO EXPLAIN RECENT ALMA IMAGES OF ASYMMETRIC `DUST-TRAPS' IN TRANSITION DISKS. HYDRODYNAMIC ACTIVITIES THUS PLAY A CRUCIAL ROLE AT EVERY STAGE OF PLANET FORMATION AND DISK EVOLUTION. WE PROPOSE TO DEVELOP THEORETICAL MODELS OF THE ABOVE HYDRODYNAMIC PROCESSES UNDER PHYSICAL DISK CONDITIONS BY PROPERLY ACCOUNTING FOR DISK THERMODYNAMICS DUST DYNAMICS DISK SELF-GRAVITY AND THREE-DIMENSIONAL EFFECTS. BY INCLUDING THESE EFFECTS WE GO WELL-BEYOND PREVIOUS WORKS BASED ON IDEALIZED DISK MODELS. THIS EFFORT IS NECESSARY TO UNDERSTAND HOW THESE INSTABILITIES OPERATE AND INTERACT IN REALISTIC PROTOPLANETARY DISKS. THIS WILL ENABLE US TO PROVIDE A UNIFIED PICTURE OF HOW VARIOUS HYDRODYNAMIC ACTIVITIES FIT TOGETHER TO DRIVE GLOBAL DISK EVOLUTION. WE WILL ADDRESS KEY QUESTIONS INCLUDING THE STRENGTH OF THE RESULTING HYDRODYNAMIC TURBULENCE THE LIFETIME OF LARGE-SCALE VORTICES UNDER REALISTIC DISK CONDITIONS AND THEIR IMPACT ON THE EVOLUTION OF SOLIDS WITHIN THE DISK. INCLUSION OF THESE ADDITIONAL PHYSICS WILL LIKELY UNCOVER NEW YET-UNKNOWN HYDRODYNAMIC PROCESSES. OUR GENERALIZED MODELS ENABLES A DIRECT LINK BETWEEN THEORY AND OBSERVATIONS. FOR EXAMPLE A SELF-CONSISTENT INCORPORATION OF DUST DYNAMICS INTO THE THEORY OF HYDRODYNAMIC INSTABILITIES IS PARTICULARLY IMPORTANT SINCE IT IS THE DUST COMPONENT THAT IS USUALLY OBSERVED. WE WILL ALSO ESTABLISH THE CONNECTION BETWEEN THE PROPERTIES OF LARGE-SCALE OBSERVABLE STRUCTURES SUCH AS VORTICES TO THE UNDERLYING DISK PROPERTIES SUCH AS DISK MASS AND VERTICAL STRUCTURE WHICH ARE DIFFICULT TO INFER DIRECTLY FROM OBSERVATIONS. WE ALSO PROPOSE TO STUDY FOR THE FIRST TIME THE DYNAMICAL INTERACTION BETWEEN HYDRODYNAMIC TURBULENCE AND PROTO-PLANETS AS WELL AS THE INFLUENCE OF LARGE-SCALE VORTICES ON DISK-PLANET INTERACTION. THIS IS NECESSARY TOWARDS A REALISTIC MODELING OF THE ORBITAL EVOLUTION OF PROTO PLANETS AND THUS IN PREDICTING THE FINAL ARCHITECTURE OF PLANETARY SYSTEMS. THE PROPOSAL TEAM'S EXPERTISE AND EXPERIENCE RANGING FROM MATHEMATICAL ANALYSES TO STATE-OF THEART NUMERICAL SIMULATIONS IN ASTROPHYSICAL FLUID DYNAMICS PROVIDES A MULTI-METHOD APPROACH TO THESE PROBLEMS. THIS IS NECESSARY TOWARDS ESTABLISHING A RIGOROUS UNDERSTANDING OF THESE FUNDAMENTAL HYDRODYNAMICAL PROCESSES IN PROTOPLANETARY ACCRETION DISKS.