THE DISCOVERY OF FAST RADIO BURSTS (FRBS) - INTENSE PULSES OF RADIO EMISSION LASTING A FEW MILLISECONDS - HAS OPENED A NEW WINDOW INTO HIGH-ENERGY ASTROPHYSICS. BECAUSE THEIR DISPERSION MEASURE (COLUMN DENSITY OF FREE ELECTRONS ALONG THE LINE OF SIGHT) GREATLY EXCEEDS THE GALACTIC CONTRIBUTION FRBS WERE SUGGESTED TO ORIGINATE FROM COSMOLOGICAL DISTANCES. THIS WAS RECENTLY CONFIRMED BY THE DISCOVERY OF THE REPEATING FRB 121102 AND ITS LOCALIZATION TO A DWARF STAR-FORMING GALAXY AT REDSHIFT Z=0.1927. GIVEN THIS LARGE DISTANCE THE ENORMOUS IMPLIED BRIGHTNESS TEMPERATURE REQUIRES THAT FRB RADIATION BE COHERENT. OUR THEORETICAL UNDERSTANDING OF FRBS LAGS FAR BEHIND THIS OBSERVATIONAL PROGRESS WITH MAJOR UNKNOWNS INCLUDING THE PROGENITORS AND RADIATION MECHANISMS. SEVERAL WORKS HAVE SUGGESTED YOUNG MAGNETIZED NEUTRON STARS (MAGNETARS) AS PROMISING SOURCES OF FRBS. MAGNETARS CAN NATURALLY EXPLAIN THE SHORT FRB DURATIONS LARGE ENERGY REQUIREMENTS AND ORDERED MAGNETIC FIELDS NEEDED FOR COHERENT EMISSION. METZGER LED WORK SHOWING THAT THE HOST GALAXY OF FRB 121102 IS REMARKABLY SIMILAR TO THOSE HOSTING SUPERLUMINOUS SUPERNOVAE AND LONG DURATION GAMMA RAY BURSTS WHICH ALSO COULD BE POWERED BY YOUNG MAGNETARS. MOST PREVIOUS WORKS INVOKING MAGNETARS AS FRB SOURCES SIMPLY ASSUMED THAT A FRACTION OF THE FREE ENERGY IN THE SYSTEM IS RADIATED AWAY AT GHZ FREQUENCIES BY COHERENT CHARGE "BUNCHES." HOWEVER THE CONDITIONS FOR COHERENT EMISSION AND THE VERY EXISTENCE OF CHARGE BUNCHES WITH THE REQUIRED PROPERTIES ARE POSTULATED AD HOC RESULTING IN MODELS WITH LITTLE PREDICTIVE POWER. WE PROPOSE A RESEARCH PROGRAM TO PLACE THE MAGNETAR FRB MODEL ON SOLID THEORETICAL FOOTING. AN FRB MAY BE PRODUCED WHEN THE STRONGLY MAGNETIZED PULSE RELEASED DURING A MAGNETAR FLARE INTERACTS WITH THE SLOWER PRE-FLARE MAGNETAR WIND FORMING A RELATIVISTIC SHOCK. AT THE SHOCK THE DISTRIBUTION OF GYRATING PARTICLES IS UNSTABLE TO THE SYNCHROTRON MASER INSTABILITY. THIS RESULTS IN THE STIMULATED EMISSION OF ELECTROMAGNETIC WAVES POWERING THE FRB. THANKS TO KEY ADVANCES IN NUMERICAL ALGORITHMS AND COMPUTER CAPABILITIES LED IN PART BY SIRONI THE MULTI-DIMENSIONAL PHYSICS OF THE SYNCHROTRON MASER CAN NOW BE CAPTURED FROM FIRST PRINCIPLES WITH PARTICLE-INCELL (PIC) CODES. WE WILL PERFORM A SUITE OF 2D AND 3D PIC SIMULATIONS OF RELATIVISTIC MAGNETICALLY-DOMINATED SHOCKS UNDER CONDITIONS APPROPRIATE FOR MAGNETAR WINDS. BY VARYING THE SHOCK LORENTZ FACTOR AND THE FLOW MAGNETIZATION TEMPERATURE AND COMPOSITION (BOTH PAIR AND PAIR-PROTON PLASMAS SINCE THE EJECTA OF THE MAGNETAR FLARE COULD BE BARYON-DOMINATED) WE WILL QUANTIFY THE DEPENDENCE OF THE FRB EFFICIENCY SPECTRUM AND POLARIZATION ON THE LOCAL PLASMA CONDITIONS. FOLLOWING ITS CREATION THE FRB PULSE PROPAGATES THROUGH THE SURROUNDING PLASMA OF THE MAGNETAR NEBULA AND SUPERNOVA EJECTA ON ITS WAY TO EARTH. BUILDING ON THE EXPERIENCE OF METZGER IN EXPLORING SIMILAR ENVIRONMENTS WE WILL ASSESS THE INFLUENCE OF PROPAGATION ON THE PULSE SPECTRUM INTENSITY AND POLARIZATION ANGLE. THE PROPERTIES OF THE INCIDENT RADIO WAVES WILL BE MOTIVATED DIRECTLY FROM THE RESULTS OF OUR PIC SIMULATIONS. THE COMBINATION OF AB INITIO PIC SIMULATIONS WITH RADIATIVE TRANSFER CALCULATIONS WILL ENABLE US TO ANSWER SEVERAL KEY QUESTIONS: WITH WHAT EFFICIENCY IS THE BULK ENERGY OF THE MAGNETAR FLARE CONVERTED INTO COHERENT RADIO EMISSION? WHAT IS THE PREDICTED FRB SPECTRUM AND POLARIZATION? HOW DO THE FRB PROPERTIES CONSTRAIN THE COMPOSITION AND MAGNETIZATION OF MAGNETAR WINDS? ITS DIVERSE COMBINATION OF THEORETICAL AND NUMERICAL EXPERTISE PROVIDES OUR GROUP WITH A UNIQUE OPPORTUNITY TO DEVELOP A SELFCONSISTENT MODEL OF FRB EMISSION WHICH WILL SUPPORT (OR CHALLENGE!) THE MAGNETAR MODEL AND PROVIDE TESTABLE PREDICTIONS FOR THE WIDE ARRAY OF FRB SURVEYS COMING ONLINE IN THE NEAR FUTURE.