MOST M DWARF FLARES EXHIBIT A STRONG RESPONSE IN THE X-RAY AND NUV IN LINE WITH THE NEUPERT EFFECT AND THE STANDARD HEATING SCENARIO FOR LESS ENERGETIC SOLAR FLARES. HOWEVER SOME FLARES PRODUCE ONLY BRIGHT X-RAYS (QUASI-NEUPERT) AND OTHERS ONLY A BRIGHT NUV RESPONSE (NON-NEUPERT). OUR FUNDAMENTAL UNDERSTANDING OF STELLAR FLARES IS HAMPERED BY THE LACK OF MULTI-WAVELENGTH OBSERVATIONAL DATA THAT CAN ROBUSTLY CONSTRAIN THE PHYSICS IN STATE-OF-THE-ART MODELS. WE PROPOSE A LARGE 450 KS XMM CAMPAIGN TO DETERMINE THE ORIGIN OF NEUPERT VERSUS NON-NEUPERT FLARES IN AU MIC. OUR 8X INCREASE IN XMM COVERAGE AND FIRST CONTEMPORANEOUS MULTI- WAVELENGTH STUDY OF THE SYSTEM WILL RESULT IN 50 FLARES. THE TIMING AND AMPLITUDE OF THE X-RAY NUV AND OPTICAL BEHAVIOR OF THESE FLARES WILL DETERMINE WHETHER THE DIFFERENCES ARE RELATED TO THE RELATIVE ROLE OF PROTON AND ELECTRON BEAMS IN THE EVENTS. THIS STUDY WILL ALSO CONSTRAIN THE HIGH-ENERGY TAIL OF AU MIC'S FLARE FREQUENCY HENCE ENABLE A TEST OF WHETHER THE SYSTEM'S DEBRIS DISK IS EXPERIENCING SPACE-WEATHER.