INCREASINGLY SOPHISTICATED INSTRUMENTS AND NUMERICAL SIMULATIONS HAVE REVEALED A WIDE VARIETY OF KINETIC PROCESSES AND MULTISCALE STRUCTURES IN EARTH S DAYSIDE MAGNETOPAUSE BOUNDARY LAYERS THE REGIONS FORMED BY THE MAGNETOSHEATH BOUNDARY LAYER (MSBL) AND THE LOW LATITUDE BOUNDARY LAYER (LLBL). BOTH OBSERVATIONS AND SIMULATIONS INDICATE THAT FOR SOUTHWARD INTERPLANETARY MAGNETIC FIELD (IMF) KINETIC PROCESSES ARE LIKELY TO CONTRIBUTE TO PLASMA ENERGIZATION AS THE PLASMA CROSSES THE RECONNECTION SEPARATRICES THAT SEPARATE THE OUTFLOW REGIONS FROM THE INFLOW REGIONS. HOWEVER IT IS UNKNOWN HOW FAR FROM THE DIFFUSION REGIONS WE SHOULD EXPECT SUCH ENERGIZATION TO OCCUR. IN ADDITION WHILE IT IS EXPECTED THAT SECONDARY RECONNECTION LEADING TO FORMATION OF MULTISCALE STRUCTURES (E.G. MAGNETIC FLUX ROPES) PLAYS AN IMPORTANT PART IN ENERGY CONVERSION AT THE MAGNETOPAUSE ITS IMPORTANCE FOR OVERALL ENERGIZATION IN THE MAGNETOPAUSE BOUNDARY LAYERS IS UNDETERMINED. TO INVESTIGATE THESE ISSUES WE PROPOSE A THREE-YEAR INVESTIGATION THAT FOCUSES ON KINETIC PROCESSES AND MULTISCALE STRUCTURES OCCURRING IN THE MAGNETOPAUSE BOUNDARY LAYERS FORMED BY RECONNECTION OUTFLOWS FOR SOUTHWARD IMF. OUR SCIENTIFIC GOAL IS TO DETERMINE HOW PLASMA DISTRIBUTIONS AND ELECTROMAGNETIC FIELDS AS WELL AS FILAMENTARY STRUCTURES TAKE SHAPE AND EVOLVE IN THE MAGNETOPAUSE BOUNDARY LAYERS FOR DIFFERENT SOLAR WIND PLASMA PARAMETERS AND MAGNETIC FIELD SHEARS. DEVELOPING A COMPREHENSIVE UNDERSTANDING OF THE STRUCTURE AND DYNAMICS OF THE MAGNETOPAUSE BOUNDARY LAYERS IS A CHALLENGING PROBLEM. ONE MAJOR DIFFICULTY IS THAT IT REQUIRES RESOLVING THE RECONNECTION PROCESS OCCURRING IN THE DIFFUSION REGION AS WELL AS THE DEVELOPMENT OF KINETIC PROCESSES NEAR THE SEPARATRICES AND THE EVOLUTION OF ELECTROMAGNETIC STRUCTURES FAR AWAY FROM IT. TO ADDRESS THIS MULTISCALE PROBLEM WE PROPOSE TO CARRY OUT SIMULATION STUDIES USING IMPLICIT PARTICLE-IN-CELL (IPIC3D) SIMULATIONS THAT ARE EMBEDDED IN GLOBAL MAGNETOHYDRODYNAMIC (MHD) SIMULATIONS. THESE PIC SIMULATIONS WILL BE AUGMENTED BY USING LARGE SCALE KINETIC (LSK) SIMULATIONS TO FOLLOW THE HISTORY OF GROUPS OF PARTICLES INSIDE THE SIMULATION DOMAINS. PHYSICAL PROCESSES AND STRUCTURES IDENTIFIED IN THE SIMULATIONS WILL BE VALIDATED BY THE STUDY OF OUTFLOW EVENTS OBSERVED BY THE MAGNETOSPHERIC MULTISCALE (MMS) SPACECRAFT AT THE DAYSIDE MAGNETOPAUSE. ADDITIONAL OBSERVATIONS FROM SPACECRAFT SUCH AS CLUSTER WILL BE USED TO PROVIDE SUPPORTING INFORMATION IN PARTICULAR WHEN STUDYING THE LARGE-SCALE EVOLUTION FAR FROM THE RECONNECTION DIFFUSION REGIONS. BECAUSE MAGNETIC RECONNECTION PROCESSES ARE UBIQUITOUS IN THE UNIVERSE RECONNECTION OUTFLOWS ARE ROUTINELY OBSERVED IN THE HELIOSPHERE SUCH AS AT PLANETARY MAGNETOPAUSES MAGNETOTAILS AND IN LESS EXPECTED REGIONS SUCH AS IN THE SOLAR WIND AND IN THE MAGNETOSHEATH. HENCE BY ADDRESSING THE STRUCTURE AND DYNAMICS OF THE BOUNDARY LAYERS FORMED BY RECONNECTION OUTFLOWS AT EARTH S MAGNETOPAUSE THE PROPOSED RESEARCH WILL DIRECTLY ADDRESS THE HIGH-LEVEL SCIENCE GOALS 3 AND 4 FROM THE HELIOPHYSICS DECADAL SURVEY: DETERMINE THE INTERACTION OF THE SUN WITH THE SOLAR SYSTEM AND THE INTERSTELLAR MEDIUM AND DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE.