IN THE EVOLUTION OF A CORONAL MASS EJECTION (CME) AND THE ASSOCIATED SOLAR FLARE A CURRENT SHEET CONNECTING THE CME TO THE POSTERUPTION FLARE ARCADE IS CRITICAL AS THE LOCATION OF MAGNETIC RECONNECTION AND ENERGY RELEASE FOR THE FLARE. NUMEROUS OBSERVATIONS IN UV EUV AND X-RAYS INDICATE THE PRESENCE OF HEATED PLASMAS SURROUNDING/WITHIN THE CURRENT SHEETS. ALTHOUGH NUMERICAL MODELS CAN REPRODUCE THE TEMPERATURES AND GENERAL APPEARANCE OF THE SHEET STRUCTURES AND SOME OF THE SMALLER-SCALE FLOWS IT IS ONLY RECENTLY THAT HIGH-RESOLUTION OBSERVATIONS HAVE BECOME AVAILABLE FOR QUANTITATIVELY SCRUTINIZING THE CONDITIONS WITHIN THE SHEET AREA. DATA FROM HINODE AND SDO REVEAL AN ENVIRONMENT FAR MORE COMPLEX THAN THE SIMPLE LAMINAR CURRENT SHEET ENVISIONED IN TWO-DIMENSIONAL AND 2.5-D MODELS OF RECONNECTION. INDEED OUR ANALYSES STEMMING FROM PRIOR NASA GRANTS DEMONSTRATE THAT THE PLASMA BETA IN THE CURRENT SHEET IS OF ORDER UNITY SO THAT GAS PRESSURE FORCES AND MAGNETIC TENSIONS HAVE SIGNIFICANT AND IMPORTANT INTERPLAY IN THIS CRUCIAL REGION. THESE COMPLEX DYNAMIC VARIATIONS IN TEMPERATURE DENSITY AND VELOCITY DIRECTLY AFFECT THE RATE OF MAGNETIC RECONNECTION IN THE CURRENT SHEETS AND SO A QUANTITATIVE CHARACTERIZATION OF THE CONDITIONS IN AND AROUND THE CURRENT SHEETS IS VITAL TO UNDERSTANDING HOW THE ENVIRONMENT CAN BECOME CONDUCIVE TO RECONNECTION. THE PRIMARY OBJECTIVE OF THIS INVESTIGATION IS AN EMPIRICAL CHARACTERIZATION OF CONDITIONS AND PROCESSES IN THE OBSERVED PLASMA SHEETS INCLUDING TEMPORALLY AND SPATIALLY RESOLVED VARIATIONS IN TEMPERATURE DENSITY AND VELOCITY. THE TEAM WILL DETECT TRACK AND QUANTITATIVELY CHARACTERIZE SUPRA-ARCADE DOWNFLOWS (SADS) AND OTHER TURBULENT FLOWS FOR APPROXIMATELY TEN FLARES OBSERVED BY SDO/ AIA AND HINODE/XRT WHERE AVAILABLE USING SOFTWARE TOOLS DEVELOPED WITH PRIOR NASA FUNDING. THE TEAM WILL ALSO MEASURE THE TEMPERATURE-DEPENDENT DISTRIBUTION OF MASS DENSITY (I.E DIFFERENTIAL EMISSION MEASURES DEM) IN THE PLASMA SHEETS FOR THE SAME FLARES AGAIN USING TOOLS DEVELOPED WITH PRIOR NASA FUNDING. THE OBSERVATIONAL ANALYSIS BUILDS UPON OUR RECENTLY PUBLISHED FINDINGS TAKING MAXIMUM ADVANTAGE OF THE HIGH-RESOLUTION DATA RETURNED FROM SDO/AIA AND HINODE/XRT. THE DEM MEASUREMENTS ARE DEMONSTRABLY VALUABLE FOR UNDERSTANDING HEATING AND THERMAL CONDUCTION WITHIN THE PLASMA SHEET AS WELL AS ESTIMATES OF PLASMA BETA. THE SPEEDS AND ACCELERATIONS OF THE SADS ARE DIRECTLY LINKED TO THE SPEEDS OF RECONNECTION OUTFLOW ACCORDING TO NUMEROUS INDEPENDENT NUMERICAL MODELS; WHEREAS THE DISTRIBUTIONS OF SIZES OF SADS ARE RELEVANT TO UNDERSTANDING THE SIZES OF POST-RECONNECTION FLUX TUBES AND/OR THE BREAKUP OF RECONNECTION JETS DUE TO RAYLEIGH-TAYLOR INSTABILITIES. THE FINDINGS OF THIS INVESTIGATION ARE RELEVANT TO UNDERSTANDING THE CONDITIONS THAT INITIATE ACCELERATE AND PROLONG RECONNECTION (E.G. VOLUME DENSITY OF SECONDARY MAGNETIC ISLANDS AT SMALL LENGTH SCALES) AND DIRECTLY ADDRESS PRIORITY OBJECTIVES IN NASA'S HELIOPHYSICS ROADMAP SUCH AS SCALE SIZES AND GEOMETRIES OF RECONNECTION KINETIC PROCESSES RESPONSIBLE FOR RECONNECTION AND THE RELATIONSHIP BETWEEN MICROPHYSICAL PROCESSES AND LARGE-SCALE TOPOLOGIES. THE INVESTIGATION THUS ADDRESSES GOAL 1 OF THE DECADAL SURVEY "DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT."