FAST FOWS EMERGING FROM RECONNECTION IN THE MAGNETOTAIL HAVE BEEN STUDIED EXTENSIVELY USING MHD SIMULATIONS (E.G. BIRN ET AL. 2011) WHERE THE BREAKING OF THESE FLOWS HAS BEEN OBSERVATIONALLY ASSOCIATED WITH THE GENERATION OF KINETIC ALFVEN WAVES (E.G CHASTON ET AL. 2012) THAT CAN IN-TURN CONTRIBUTE TO THE ENERGIZATION OF ELECTRONS TO FORM THE BROADBAND AURORA. MHD STUDIES ALONE LACK THE KINETIC ELECTRON PHYSICS NEEDED TO UNDERSTAND HOW ENERGY INCIDENT IN THE FLOWS COUPLES TO ELECTRON ENERGIZATION. ON THE OTHER HAND KINETIC SIMULATIONS ARE UNABLE TO ADDRESS THE GLOBAL SCALE SOLAR-WIND-MAGNETOSPHERE INTERACTION THAT IS DRIVING THE RECONNECTION AND THE FLOWS. WITH THESE MOTIVATIONS IN MIND THE AIM OF THIS PROPOSAL IS TO CHAIN SIMULATIONS OF THE LYON-FEDDER MOBBARY (LFM) GLOBAL MHD MODEL AND THE HYBRID GYROUID-KINETIC ELECTRON (GKE) MODEL CONSTRAINED BY AND COMPARED WITH SATELLITE OBSERVATIONS TO GAIN A BETTER UNDERSTANDING OF HOW THE BREAKING OF FAST FLOWS LEADS TO THE FORMATION OF THE BROADBAND AURORA. WE WILL PARTICULARLY ADDRESS THE FOLLOWING SCIENCE QUESTIONS: HOW DOES THE ENERGY IN THE FAST FLOWS COUPLE FIRST TO ALFVEN WAVES AND THEN TO ELECTRON ENERGIZATION BOTH IN THE PLASMA SHEET AND AT AURORAL ALTITUDES?; HOW DOES PRECIPITATING ELECTRON FLUX VARY WITH THE FLOW SPEED?; TO WHAT EXTENT DOES THE ELECTRON ENERGIZATION LEAD TO DAMPING OF WAVE ENERGY IN THE FLOWS? AND WHAT IS THE DISTRIBUTION OF POYNTING FLUX ELECTRON UX AND PARALLEL POTENTIAL ALONG AURORAL FIELD LINES? THE MODELS ARE IDEAL FOR THIS INVESTIGATION BECAUSE GKE HAS A WELL-ESTABLISHED HISTORY IN THE STUDY OF ALFVEN WAVE-INDUCED ELECTRON ACCELERATION IN THE EARTH'S MAGNETOSPHERE WHILE THE LFM IS ONE OF THE PRINCIPAL GLOBAL MAGNETOSPHERIC MHD MODELS AND HAS AN ESTABLISHED HISTORY IN QUANTIFYING THE DISTRIBUTION OF ALFVENIC POYNTING FLUX IN THE MAGNETOSPHERE AND IDENTIFYING THE ROLE OF THIS UX IN REGULATING MAGNETOTAIL DYNAMICS (ZHANG ET AL. 2012 2014). IN THE EXECUTION OF THIS STUDY CLUSTER AND THEMIS OBSERVATIONS WILL BE USED TO CHOOSE A HANDFUL OF EVENTS THAT EXHIBIT ALFVENIC ACTIVITY GENERATED IN THE PRESENCE OF RECONNECTION INDUCED FAST FLOWS (SUCH AS DURING SUBSTORMS). THE CORRESPONDING SOLAR WIND DATA (SOURCED FROM UPWIND MONITORS SUCH AS THE ACE SATELLITE) WILL BE USED TO DRIVE THE GLOBAL MHD SIMULATIONS AND THE ALFVENIC PERTURBATIONS EXTRACTED FROM THESE SIMULATIONS WILL THEN BE USED AS INPUT TO THE ION-GYROUID COMPONENT OF THE GKE MODEL TO UNDERSTAND HOW THE ENERGY FROM THE RECONNECTED FLUX CASCADES TO SMALLER SCALES AND ENERGIZES THE KINETIC ELECTRONS. THE CHARACTERISTICS OF THE WAVE FIELDS AND ACCELERATED ELECTRON DISTRIBUTIONS IN THE GKE SIMULATION DOMAIN WILL THEN BE COMPARED WITH THOSE EVIDENT IN RELEVANT THEMIS AND CLUSTER OBSERVATIONS TO TEST THE VALIDITY OF THE MODEL FRAMEWORK AND UNDERSTAND THE FORMATION AND EVOLUTION OF THE OBSERVED FEATURES. THIS SYSTEMATIC AND COMBINED APPROACH WILL YIELD A UNIQUE CAPABILITY TO UNDERSTAND THE GENERATION OF THE ALFVENIC AURORA.