GOALS: ULTRA LOW FREQUENCY (ULF) WAVES INTERACT WITH THE RADIATION BELTS AND POTENTIALLY AFFECT SPACE WEATHER BY GENERATING ENHANCEMENTS/DEPLETIONS IN ENERGETIC ELECTRONS THAT AFFECT SATELLITE ELECTRONICS. ULF WAVE INTERACTIONS WITH ENERGETIC ELECTRONS ARE OFTEN REPRESENTED USING A RADIAL DIFFUSION APPROXIMATION. HOWEVER SEVERAL MODELS PREDICT NON-DIFFUSIVE PARTICLE DYNAMICS IN THE PRESENCE OF LARGE SCALE MONOCHROMATIC (LSM) ULF WAVES E.G. DRIFT RESONANCE BULK RADIAL TRANSPORT ON TIMESCALES FASTER THAN RADIAL DIFFUSION AND LOCALIZED PEAKS IN PHASE SPACE DENSITY (PSD). UNTIL RECENTLY THERE WERE FEW OBSERVATIONAL CONSTRAINTS TO TEST THESE PREDICTIONS. QUASI-PERIODIC FLUCTUATIONS IN THE SOLAR WIND DRIVE A RANGE OF LSM ULF WAVES IN THE MAGNETOSPHERE WITH TIMESCALES COMPARABLE TO RELATIVISTIC ELECTRON DRIFT PERIODS. INTERVALS WITH THESE FLUCTUATIONS ARE IDEAL FOR EXPERIMENTALLY TESTING MODEL PREDICTIONS OF NONDIFFUSIVE BEHAVIOR: (1) MODELS PREDICT NON-DIFFUSIVE PARTICLE DYNAMICS IN THE PRESENCE OF SUCH WAVES (2) SUCH WAVES ARE RELATIVELY EASY TO SIMULATE AND (3) WAVE PROPERTIES CAN BE OBSERVED OVER LARGE REGIONS OF THE MAGNETOSPHERE. THIS PROPOSAL IS FOCUSED ON ADDRESSING THE OVER-ARCHING SCIENCE QUESTION DO LSM ULF WAVES ROUTINELY PRODUCE NON-DIFFUSIVE BEHAVIOR IN THE EARTH S OUTER ELECTRON RADIATION BELT? WE WILL COMBINE OBSERVATIONS AND SIMULATIONS TO CONFIRM THE PRESENCE/ABSENCE OF THREE NON-DIFFUSIVE BEHAVIORS DURING LSM ULF WAVE EVENTS DRIVEN BY SOLAR WIND FLUCTUATIONS: DRIFT RESONANCE RAPID RADIAL TRANSPORT AND RADIALLY LOCALIZED PSD PEAKS. MISSION DATA AND MODELS: OUR PRIMARY DATASETS ARE ENERGETIC PARTICLE DATA FROM THE MAGNETIC ELECTRON ION SPECTROMETER (MAGEIS) INSTRUMENT ON NASA S VAN ALLEN PROBES SPACECRAFT (RBSP) AND MAGNETIC FIELD/PLASMA MOMENT MEASUREMENTS FROM NASA S WIND ACE AND ARTEMIS MISSIONS. OTHER DATASETS INCLUDE EFW AND EMFISIS ON RBSP AS WELL AS ADDITIONAL MAGNETIC FIELD (AND WHERE AVAILABLE ELECTRIC FIELD) MEASUREMENTS FROM NASA S THEMIS AND MMS SATELLITES NOAA GOES SATELLITES ESA CLUSTER SATELLITES AND GROUND MAGNETOMETERS. FINALLY WE SHALL USE THE COMPREHENSIVE INNER MAGNETOSPHERE-IONOSPHERE (CIMI) MODEL TO COMPARE WITH MEASUREMENTS AND OBTAIN GLOBAL CONTEXT. DATA ANALYSIS/METHODOLOGY: WE WILL USE WIND/ACE/ARTEMIS DATA TO IDENTIFY PERIODS WITH QUASI-PERIODIC SOLAR WIND FLUCTUATIONS THEN USE MAGEIS DATA TO RECORD PSD PROFILES AND RESIDUAL FLUXES. A RANDOM SUBSET OF EVENTS WILL BE SIMULATED USING CIMI AND SIMULATION OUTPUT WILL BE COMPARED WITH GLOBAL WAVE MEASUREMENTS. SIMULATIONS WITH THE BEST AGREEMENT WITH MEASUREMENTS WILL BE FURTHER EXAMINED BY COMPARING SIMULATED AND OBSERVED PSD PROFILES/RESIDUAL FLUXES AT THE RBSP SATELLITE LOCATIONS AS WELL AS EXAMINING THESE QUANTITIES THROUGHOUT THE SIMULATION DOMAIN. USING ESTABLISHED TESTS BOTH OBSERVATIONS AND SIMULATIONS WILL BE USED TO DETERMINE WHETHER THE ULF WAVES ROUTINELY DRIVE DRIFT RESONANCE RAPID RADIAL TRANSPORT AND RADIALLY LOCALIZED PSD PEAKS. RELEVANCE: OUR SCIENCE QUESTION ADDRESSES THE DECADAL SURVEY GOAL DETERMINE THE DYNAMICS AND COUPLING OF THE EARTH S MAGNETOSPHERE IONOSPHERE AND ATMOSPHERE AND THEIR RESPONSE TO SOLAR AND TERRESTRIAL INPUTS. IT IS ALSO RELEVANT TO THE NASA RBSP MISSION FUNDAMENTAL OBJECTIVE TO PROVIDE UNDERSTANDING IDEALLY TO THE POINT OF PREDICTABILITY OF HOW POPULATIONS OF RELATIVISTIC ELECTRONS AND PENETRATING IONS IN SPACE FORM OR CHANGE IN RESPONSE TO VARIABLE INPUTS OF ENERGY FROM THE SUN. FINALLY IT IS RELEVANT TO THE NASA HSR INNER MAGNETOSPHERE SCIENCE AREA AS IT COMBINES MODELING AND NASA SATELLITE OBSERVATIONS. NOTE: VIRGINIA TECH IS SUBMITTING THIS PROPOSAL AND PARTICIPATING IN THIS PROJECT BASED ON THE CONDITION THAT THE RESEARCH CAN BE CONDUCTED AS FUNDAMENTAL RESEARCH. VIRGINIA TECH ANTICIPATES THERE WILL BE NO PUBLICATION APPROVAL OR OTHER REQUIREMENTS IN THE AWARD THAT WOULD RESTRICT DISCLOSURE OF THE RESEARCH RESULTS.