IN THE GIANT IMPACT THEORY THE MOON FORMED IN THE AFTERMATH OF AN OFF-CENTER COLLISION BETWEEN A PLANETARY SIZED BODY AND THE PROTO-EARTH. THE COLLISION LOFTS A RING OF DEBRIS INTO ORBIT AROUND THE EARTH AND THIS PROTO-LUNAR DISK THEN COOLS AND COALESCES TO FORM THE MOON. IN THE CANONICAL GIANT IMPACT MODELS (SEE CANUP 2004) THE IMPACTOR MASS IS COMPARABLE TO MARS AND THE ANGULAR MOMENTUM OF THE EARTH-MOON SYSTEM IS CONSERVED. THIS MODELS SUFFERS FROM AN "ISOTOPE CRISIS" (E.G. MELOSH 2014): THE MOON AND EARTH ARE ISOTOPICALLY SIMILAR WHICH IS UNEXPECTED SINCE THE MOON SHOULD CONTAIN A MATERIAL FROM AN IMPACTOR THAT LIKELY ORIGINATED ELSEWHERE IN THE SOLAR SYSTEM. IN NONCANONICAL MODELS (CUK&STEWART 2012; CANUP 2012) ANGULAR MOMENTUM OF THE EARTH-MOON SYSTEM IS REMOVED VIA AN EVECTION RESONANCE. RECENT WORK (LOCK ET AL. 2018) CONSIDERS HIGH ENERGY AND ANGULAR MOMENTUM IMPACTS IN WHICH THE COLLISION OUTCOME IS A RAPIDLY ROTATING WELL-MIXED "SYNESTIA". EXISTING GIANT IMPACT SIMULATIONS USE SMOOTHED PARTICLE HYDRODYNAMICS TECHNIQUES OR AN EULERIAN GRID CODE WITH MAXIMUM RESOLUTION ~ 100KM (SEE CANUP ET AL. 2013). WE PROPOSE TO DEVELOP AND APPLY A FAST EULERIAN SCHEME BASED ON THE ATHENA++ CODE THAT IS CAPABLE OF HIGH LINEAR RESOLUTION. OUR CODE WILL INCLUDE THE OPTION TO EVOLVE AN EMBEDDED MAGNETIC FIELD IN THE MAGNETOHYDRODYNAMIC (MHD) APPROXIMATION MOTIVATED BY RECENT WORK (GAMMIE ET AL. 2016 CARBALLIDO ET AL. 2016) THAT SHOWS THAT MAGNETIC FIELDS COUPLE TO HOT VAPORIZED PARTS OF THE PROTOLUNAR DISK. WE PROPOSE THE FOLLOWING NOVEL INVESTIGATIONS OF THE GIANT IMPACT HYPOTHESIS USING NUMERICAL EXPERIMENTS: (1) BY WHAT FACTOR CAN A GIANT IMPACT AMPLIFY THE MAGNETIC FIELD OF THE TARGET AND IMPACTOR? (2) HOW DOES A MAGNETIZED MODEL DIFFER FROM AN UNMAGNETIZED CONTROL MODEL? (3) CAN A GIANT IMPACT REMNANTS LOSE ANGULAR MOMENTUM THROUGH A MAGNETIZED WIND? (4) WHAT IS THE STRUCTURE (RUN OF DENSITY TEMPERATURE COMPOSITION AND FIELD STRENGTH) OF THE BOUNDARY LAYER BETWEEN THE PROTOLUNAR DISK AND EARTH? (5) WHAT IS THE RATE OF MIXING THROUGH THE BOUNDARY LAYER? (6) WHAT IS THE RATE OF MIXING IN A PROTOLUNAR DISK THAT IS IN CONTACT WITH A DYNAMICALLY ACTIVE BOUNDARY LAYER? WE WILL ANSWER THESE QUESTIONS USING A SPECIAL BRANCH OF THE ATHENA++ ASTROPHYSICAL MHD CODE THAT WE WILL BUILD TEST AND PUBLICLY RELEASE. WE HOPE TO CREATE A TOOL THAT IS USEFUL TO COMMUNITIES INTERESTED IN MOON FORMATION GIANT IMPACTS EXOPLANET FORMATION AND OTHER IMPACT PROBLEMS THAT CAN BE TREATED IN A FLUID APPROXIMATION. THE PI HAS A RECORD OF DEVELOPING AND PUBLICLY RELEASING CODES THAT ARE WIDELY USED IN OTHER CONTEXTS. THE ATHENA++ CODE IS A RIGOROUSLY TESTED HIGHLY OPTIMIZED FRAMEWORK FOR SIMULATING ASTROPHYSICAL FLUIDS. IT IS FULLY VECTORIZED AND THEREFORE FAST IN SCALAR MODE AND IT ALSO SCALES EFFICIENTLY TO HUNDREDS OF THOUSANDS OF CORES. THIS WILL ENABLE NUMERICAL INVESTIGATION AT HIGHER RESOLUTION THAN HERETOFORE POSSIBLE. WE HAVE ADDED TABULAR EQUATION OF STATE CAPABILITY TO THE ATHENA++ CODE AND ARE IN THE PROCESS OF ADDING MATERIAL TRACKING CAPABILITY. THE WORK WILL CONSTITUTE THE PHD THESIS OF ILLINOIS GRADUATE STUDENT PATRICK MULLEN. PI GAMMIE HAS EXTENSIVE EXPERIENCE WITH NUMERICAL METHODS ASTROPHYSICAL FLUIDS AND DISK DYNAMICS. FORM NRESS-300 VERSION 3.0 APR 09 THE PROPOSED WORK IS WITHIN THE SCOPE OF THE PROGRAM ELEMENT BECAUSE "EMERGING WORLDS" AIMS TO DISCOVER HOW THE SOLAR SYSTEM FORMED AND EVOLVED AND THIS YEAR THE PLANETARY SCIENCE DIVISION IS PARTICULARLY SOLICITING PROPOSALS THAT FOCUS ON THE MOON.