ENHANCEMENTS OF>0.1 MEV/NUCLEON IONS NEAR 1 AU IN ASSOCIATION WITH THE PASSAGE OF AN INTERPLANETARY CORONAL MASS EJECTION (ICME) ARE OFTEN REFERRED TO AS ENERGETIC STORM PARTICLE (ESP) EVENTS. THESE EVENTS ARE THOUGHT TO OCCUR VIA DIFFUSIVE SHOCK ACCELERATION (DSA) AT SHOCKS DRIVEN BY FAST ICMES AS THEY PLOUGH THROUGH THE INTERPLANETARY MEDIUM. THE IONS AND ELECTRONS ENERGIZED IN THESE EVENTS CAN PRODUCE SIGNIFICANT INCREASES IN NEAR-EARTH PARTICULATE RADIATION THAT POSE SEVERE RADIATION HAZARDS TO ASTRONAUTS AND HARDWARE IN SPACE. PHYSICAL PARAMETERS THOUGHT TO AFFECT ESP PRODUCTION INCLUDE THE ICME SHOCK SPEED STRENGTH AND OBLIQUITY THE UPSTREAM SEED PARTICLE POPULATION AND INTERPLANETARY TURBULENCE AMONG OTHERS. WHILE SEVERAL OBSERVATIONAL STUDIES AND THEORIES HAVE ATTEMPTED TO LINK THE PROPERTIES OF ESPS TO THESE DRIVERS RELIABLE PREDICTION OF ESP PROPERTIES (E.G. INTENSITIES SPECTRA AND ABUNDANCES) INCLUDING THEIR EVENT-TO-EVENT AND INTRA-EVENT VARIABILITY HAS SO FAR PROVEN ELUSIVE. THIS POINTS TO AN INCOMPLETE UNDERSTANDING OF HOW ICME SHOCKS ACCELERATE ESPS IN INTERPLANETARY SPACE. OUR OVERARCHING GOAL IS TO ADVANCE CURRENT UNDERSTANDING OF ESP ACCELERATION AT INTERPLANETARY SHOCKS NEAR 1 AU. WE WILL ACHIEVE THIS GOAL BY ANSWERING THE FOLLOWING THREE SCIENCE QUESTIONS: 1. WHAT IS THE RELATIONSHIP BETWEEN LOCALLY OBSERVED SHOCK PROPERTIES AND ESP PROPERTIES SUCH AS INTENSITIES ENERGY SPECTRA AND ABUNDANCES? 2. HOW DO AMBIENT TURBULENCE LEVELS AND THE PRESENCE OF SUPRATHERMAL SEED POPULATIONS AFFECT ESP PROPERTIES? 3. WHAT CAUSES THE INTRA-EVENT VARIABILITY IN ESPS OBSERVED AT TWO OR MORE LONGITUDINALLY SEPARATED SPACECRAFT DURING SOLAR CYCLE 24? BY ADDRESSING THESE QUESTIONS WE WILL PINPOINT THE PHYSICAL PARAMETERS AND PROCESSES THAT INFLUENCE ESP PROPERTIES AND LEAD TO THEIR EVENT-TO-EVENT AND INTRA-EVENT VARIABILITY THEREBY ADVANCING CURRENT UNDERSTANDING OF ICME-DRIVEN PARTICLE ACCELERATION AT 1 AU. OUR STUDY WILL UTILIZE THE PARTICLE ACCELERATION AND TRANSPORT (PATH) MODEL TO EXAMINE THE INFLUENCE OF SHOCK PROPERTIES TURBULENCE AND SUPRATHERMAL SEED PARTICLES ON ESP PROPERTIES. THE PATH MODEL INPUTS CONSTRAINED BY OBSERVATIONS WILL BE VARIED SYSTEMATICALLY TO ISOLATE THE INFLUENCE OF EACH POTENTIAL DRIVER ON ESP INTENSITIES SPECTRA AND ABUNDANCES. PATH WILL ALSO BE USED TO MODEL SELECTED MULTI-SPACECRAFT ESP EVENTS TO HELP IDENTIFY THE MECHANISMS RESPONSIBLE FOR PRODUCING ANY INTRA-EVENT VARIATIONS. THE MODELING EFFORT WILL BE SUPPORTED BY ANALYSIS OF ENERGETIC H HE O AND FE ION SOLAR WIND PLASMA AND INTERPLANETARY MAGNETIC FIELD MEASUREMENTS FROM ACE WIND AND STEREO DURING SEVERAL (>100) ESP EVENTS OBSERVED NEAR EARTH ORBIT. THESE MEASUREMENTS WILL BE USED TO QUANTIFY THE RANGE IN THESE ESP PROPERTIES AND THEIR CORRELATION WITH LOCAL SHOCK PROPERTIES TURBULENCE AND SEED PARTICLES. THESE RESULTS WILL BE COMPARED TO RESULTS FROM PREVIOUS SOLAR CYCLES. THE RELATIONSHIPS UNCOVERED IN THESE ANALYSES ARE EXPECTED TO LEAD TO A MORE COMPLETE UNDERSTANDING OF ICME-DRIVEN PARTICLE ACCELERATION AT 1 AU. OUR PROPOSED RESEARCH DIRECTLY RESPONDS TO THE ROSES 2016 SH: HSR BY COMBINING MODELING AND DATA ANALYSIS TO ADDRESS A TOPIC RELATED TO PARTICLE ACCELERATION TRANSPORT MODULATION IN THE HELIOSPHERE . OUR RESULTS WILL SIGNIFICANTLY IMPROVE BASIC UNDERSTANDING OF THE PHYSICS OF ICME-DRIVEN PARTICLE ACCELERATION AT 1 AU WHICH STRONGLY IMPACTS A KEY STRATEGIC GOAL OF NASA S HELIOPHYSICS DIVISION I.E. UNDERSTAND THE SUN AND ITS INTERACTIONS WITH THE EARTH AND THE SOLAR SYSTEM INCLUDING SPACE WEATHER. OUR STATED OBJECTIVES ALSO RESPOND TO TWO SCIENCE GOALS OF THE 2012 SOLAR AND SPACE PHYSICS DECADAL SURVEY NAMELY (1) DETERMINE THE ORIGINS OF THE SUN S ACTIVITY AND PREDICT THE VARIATIONS OF THE SPACE ENVIRONMENT AND (4) DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE.