OBJECTIVES: THE VOYAGER INTERSTELLAR MISSION OFFERS A UNIQUE OPPORTUNITY TO STUDY THE REGION OF SPACE ON THE FAR SIDE OF THE HELIOPAUSE KNOWN AS THE OUTER HELIOSHEATH (OHS). THE PHYSICAL PROPERTIES OF THE OHS ARE VERY DIFFERENT FROM THOSE OF THE SOLAR WIND OR THE SURROUNDING INTERSTELLAR CLOUD. IN PARTICULAR COMPRESSIVE STRUCTURES THOUGHT TO BE SHOCK WAVES HAVE RAMPS THAT ARE THOUSANDS OF TIMES BROADER THAN THEIR COUNTERPARTS IN THE SOLAR WIND. TURBULENT MAGNETIC FLUCTUATIONS IN THE OHS HAVE EXTREMELY LARGE SPATIAL SCALES WELL IN EXCESS OF THE LARMOR RADII OF THE DOMINANT ENERGETIC PARTICLE SPECIES WHICH HAS CRITICAL CONSEQUENCES FOR COSMIC RAY INTENSITY VARIATIONS AND ANISOTROPIES. IN ADDITION PICKUP ION POPULATIONS GENERATED IN THE OHS FROM ATOMS OF HELIOSPHERIC ORIGIN HAVE A DIFFERENT PATTERN OF INTERACTION WITH AMBIENT AND IN SITU GENERATED TURBULENCE THAN THE IONS OF INTERSTELLAR OR COMETARY ORIGIN. THE PRIMARY OBJECTIVE OF THIS PROPOSAL IS TO INTERPRET AND EXPLAIN THE VOYAGER MAGNETIC FIELD AND COSMIC-RAY MEASUREMENTS AND LINK THESE OBSERVATIONS WITH THE IBEX REMOTE SENSING OBSERVATIONS OF ENERGETIC NEUTRALS GENERATED IN THE OHS. THE PROJECT WILL ADDRESS THE FOLLOWING SCIENCE QUESTIONS: "WHY ARE SHOCK WAVES OBSERVED IN THE OHS ARE SO MUCH BROADER THAN THEY ARE IN THE SOLAR WIND" "WHAT IS THE ORIGIN OF THE TURBULENT FLUCTUATIONS AND HOW DO THEY AFFECT PICKUP ION POPULATIONS IN THE OHS" AND "WHAT CAUSES GALACTIC COSMIC-RAY ANISOTROPIES TO VARY WITH TIME AND WHAT IS THEIR CONNECTION WITH THE GLOBAL AND LOCAL PLASMA FLOW FEATURES". THE PROJECT AIMS TO ELUCIDATE THE INTERCONNECTION BETWEEN THE MAGNETIC FIELD DATA WHICH HAS A "LOCAL" CHARACTER THE HIGHLY MOBILE COSMIC RAYS THAT SAMPLE VAST REGIONS OF SPACE ALONG MAGNETIC FIELD LINES AND NEUTRAL POPULATIONS REVEALING KINETIC SCALE PHYSICS OF THE OHS PLASMA. RELEVANCE: THE OHS IS THE REGION WHERE DIRECT COUPLING BETWEEN THE SOLAR WIND AND THE INTERSTELLAR MEDIUM OCCURS. THE TOPIC IS THEREFORE IMMEDIATELY RELEVANT TO SCIENCE GOALS 3 AND 4 OF THE OF THE HELIOPHYSICS DECADAL SURVEY. THE PROJECT WILL ADDRESS THE FUNDAMENTAL LONG-STANDING PROBLEMS OF INTERSTELLAR MEDIUM TURBULENCE STABILITY OF HIGHLY ANISOTROPIC ION DISTRIBUTIONS AND THE PHYSICS OF CHARGED PARTICLE TRANSPORT IN TURBULENT ENVIRONMENTS. THE PROJECT IS WELL POSITIONED TO MAKE A DECISIVE IMPACT ON OUR UNDERSTANDING OF THE OUTER HELIOSHEATH AND OUR IMMEDIATE INTERSTELLAR ENVIRONMENT AND HAS POTENTIAL FOR BROADER IMPACTS IN BOTH HELIOSPHERIC AND ASTROPHYSICAL CONTEXTS. METHODOLOGY: THE PROJECT WILL UTILIZE INSTRUMENT DATA FROM THE VOYAGER 1 AND 2 SPACE PROBES INCLUDING MAGNETOMETER (MAG) DATA AND THE DATA FROM THE LECP AND CRS CHARGED PARTICLE DETECTORS. THE TEAM HAS A PROVEN TRACK RECORD OF WORKING WITH VOYAGER DATA HAVING PREVIOUSLY ANALYZED AND MODELED THE ENERGETIC PARTICLE ANISOTROPIES NEAR THE HELIOPAUSE AND HELPED UNCOVER THE SPECTRUM OF MAGNETIC TURBULENCE IN THE OHS DEDUCED FROM 1.5 YEARS OF MAG OBSERVATIONS. THE MEASURED WIDTH AND INTENSITY PROFILE OF THE IBEX RIBBON WILL BE USED TO DEDUCE THE GEOMETRY OF THE MAGNETIC FIELD INCLUDING LARGE-SCALE AND KINETIC SCALE FLUCTUATIONS USING COMPUTER MODELS. MODELING EFFORTS WILL CONSIST OF GLOBAL MHD-NEUTRAL SIMULATIONS OF THE HELIOSPHERE TO REVEAL THE MAGNETIC DRAPING PATTERN KINETIC (HYBRID QUASI-NEUTRAL AND FULL ELECTRON-ION PARTICLE-MESH IF REQUIRED) SIMULATIONS OF SHOCK WAVES TRAVELING IN AN OHS PLASMA AND OF PICKUP ION RING LIKE POPULATIONS AND ENERGETIC PARTICLE TRANSPORT SIMULATIONS OF GALACTIC COSMIC RAYS IN THE PRESENCE OF LARGE-SCALE FIELD DRAPING AS WELL AS BROAD RAMP SHOCK WAVES AND COMPRESSIVE STRUCTURES AS PART OF THE AMBIENT TURBULENCE. THE TEAM HAS EXPERIENCE WITH ALL THREE TYPES OF MODELS HAVING APPLIED THEM PREVIOUSLY TO THE SOLAR WIND AND INNER HELIOSHEATH REGIONS.