GOALS: ALTHOUGH IN SITU OBSERVATIONS OF THE SOLAR WIND ARE INTRINSICALLY LOCAL WHEN YOU COMBINE PLASMA FIELD AND COMPOSITION OBSERVATIONS YOU CAN FIND INFORMATION ABOUT THE SOLAR WIND SOURCES ACCELERATION AND THE DYNAMIC INTERACTION THAT OCCURS IN TRANSIT FROM THE SUN TO POINT OF OBSERVATION. WE SEEK TO DIFFERENTIATE THE SOURCE ACCELERATION AND DYNAMIC PROCESSING FOR THE FAST-SLOW WIND BOUNDARIES. QUESTIONS: Q1) ARE THERE PLASMA AND FIELD SIGNATURES IN FAST-SLOW WIND TRANSITIONS THAT CORRESPOND SO WELL WITH HEAVY ION COMPOSITION BOUNDARIES THAT WE CAN DISTINGUISH THE SOURCE PROPERTIES IN THE PLASMA AND FIELD MEASUREMENTS FROM THE DYNAMIC INTERACTION PROPERTIES? Q2) DO THE FAST-SLOW WIND TRANSITIONS HAVE DIFFERENT SIGNATURES DEPENDING ON THE SIZE OF ADJACENT FAST STREAMS (CORONAL HOLES)? Q3) HOW DO THE PLASMA FIELD AND HEAVY ION COMPOSITION SIGNATURES IN FAST-SLOW WIND TRANSITIONS CHANGE WITH DISTANCE FROM THE SUN? MOTIVATION: AS THE SUN ROTATES DIFFERENT FEATURES ON THE SUN EMIT PARCELS OF SOLAR WIND OF VARYING SPEEDS THAT MOVE RADIALLY AWAY FROM THE SUN AND SUBSEQUENTLY OBSERVED AS A SERIES OF FAST AND SLOW STREAMS. THE BIMODAL VIEW OF THE SOLAR WIND HAS PROVIDED THE BASIC FRAMEWORK FOR RELATING THE SOLAR WIND TO REMOTE SENSING SOLAR OBSERVATIONS. IT HAS BECOME CLEAR THAT THE FAST WIND IS ASSOCIATED WITH THE CORONAL HOLES AND THAT THE SLOW WIND WHICH IS HIGHLY VARIABLE MAY HAVE SEVERAL SOURCES (E.G. STREAMERS PSEUDOSTREAMERS BOUNDARIES OF CORONAL HOLES). WHILE THIS BIMODAL VIEW OF THE SOLAR WIND DOES EXPLAIN THE GLOBAL NATURE OF THE SOLAR WIND AT SOLAR MINIMUM (FIGURE 1) IT DOES NOT FULLY EXPLAIN THE PHYSICAL MECHANISMS THAT PRODUCE THE FAST-SLOW WIND BOUNDARY IN THE IN SITU MEASUREMENTS. SOME OF THE BOUNDARIES MAY DEVELOP IN THE CORONA AS THE SOLAR WIND IS HEATED AND ACCELERATED AS OPPOSED TO DEVELOPING IN THE CHROMOSPHERE AND PHOTOSPHERE. ANALYSIS OF SOLAR WIND OBSERVATIONS AT 1 AU SHOW CLEAR SIGNS THAT THE SOLAR WIND HAS BEEN PROCESSED ON ITS JOURNEY FROM THE SUN AND THE FAST-SLOW WIND TRANSITION AT 1 AU IS NOT AS WELL ORGANIZED AS IT IS CLOSER TO THE SUN AS OBSERVED BY HELIOS. THE FAST-SLOW WIND TRANSITION REFLECTS NOT ONLY A BOUNDARY BASED ON CONDITIONS AND PROCESSES AT THE SUN OR IN THE CORONA BUT ALSO HOW FAST AND SLOW WIND PARCELS DYNAMICALLY INTERACT EN ROUTE. WE PROPOSE TO ANALYZE FAST-SLOW WIND TRANSITIONS BY COMBINING SOLAR WIND PLASMA INTERPLANETARY MAGNETIC FIELD (IMF) AND COMPOSITION SOLAR WIND OBSERVATIONS WITHOUT AVERAGING OVER KEY FEATURES. OUR TECHNIQUES EXTRACT AND PRESERVE SEPARATE ASPECTS OF THE FAST-SLOW WIND TRANSITIONS RELATED TO THE WIND ORIGIN AND ACCELERATION FROM THOSE RELATED TO DYNAMIC PROCESSING AS THE WIND PROPAGATES. RELEVANCE TO NASA AND GI: OUR MAIN OBJECTIVE TO FURTHER OUR UNDERSTANDING OF THE FAST-SLOW WIND BOUNDARY IS CLOSELY ALIGNED WITH GOAL 4 IN THE HELIOPHYSICS DECADAL SURVEY TO DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE. THIS PROJECT USES DATA FROM ACE AND STEREO WHICH ARE CURRENT NASA FUNDED MISSIONS AND USES DATA FROM PRIOR HELIOS AND ULYSSES MISSIONS. WE USE FIELD AND PLASMA OBSERVATIONS FROM ACE STEREO ULYSSES AND HELIOS AND COMPOSITION DATA FROM ACE STEREO AND ULYSSES. OUR WORK LEVERAGES DATA FROM A WIDE RANGE OF INSTRUMENTS ON CURRENT AND PAST NASA MISSIONS TO MAXIMIZE THE RETURN WHICH IS CONSISTENT WITH THE OBJECTIVES OF THE GI PROGRAM. OUR TECHNIQUES CAN BE ADAPTED TO ANALYZE AND COMPARE SPP DATA TO SO OBSERVATIONS AS WELL AS TO COMPARE SPP AND SO DATA TO SOLAR WIND OBSERVATIONS TAKEN NEAR EARTH. IN ANSWERING QUESTION 3 ANY RADIAL TRENDS IN THE RELATIONSHIP BETWEEN THE COMPOSITION AND THE PLASMA AND FIELD MEASUREMENTS WE FIND WILL ALLOW US TO EXTRAPOLATE AND MAKE TO PREDICTIONS FOR SO AND SPP.