AT 1 AU FAST SOLAR WINDS HAVE LARGE AMPLITUDE AND CORRELATED VELOCITY AND MAGNETIC FIELD FLUCTUATIONS THAT FORM A TURBULENT ENERGY CASCADE WITH A HIGH DISSIPATION AND HEATING RATE. THESE FLUCTUATIONS ARE FOUND NEARLY UBIQUITOUSLY THROUGHOUT FAST WINDS. THESE FLUCTUATIONS ARE ALSO LARGE COMPARED TO THE VARIATION OF BACKGROUND CONDITIONS IN FAST WINDS. THE ORIGIN OF THE FAST WINDS WITH CORONAL HOLES AT THE SUN IS WELL ESTABLISHED. SLOW WINDS ARE GENERALLY SO OPPOSED IN ALL THESE RESPECTS WITH FAST WINDS THAT A DIFFERENT ORIGIN IS DEEMED LIKELY. SLOW WINDS ARE CHARACTERIZED BY CONSIDERABLE VARIABILITY IN PROPERTIES. THEY DISPLAY A WIDE RANGE OF ION TEMPERATURES AND HAVE A HIGHLY VARIABLE HELIUM TO HYDROGEN DENSITY RATIO THAT VARIES WITH THE SOLAR CYCLE. THE TURBULENT FLUCTUATIONS IN SLOW WINDS CAN REACH SMALLER AMPLITUDES AND STILL PROVIDE PLASMA HEATING. THE TURBULENT ENERGY CASCADE MUST REMAIN EFFICIENT IN THESE CIRCUMSTANCES BUT THE NATURE OF THE TURBULENT FLUCTUATIONS AND TURBULENT AND KINETIC PROCESSES THAT OPERATE HERE REMAIN TO BE SPECIFIED. THE ORIGIN OF THE SLOW WINDS HAS ALSO NOT BEEN ESTABLISHED AND CONTRIBUTIONS COULD ARISE WITH CORONAL HOLE BOUNDARIES SMALLER CORONAL HOLES ACTIVE REGIONS AND CLOSED FIELD REGIONS THAT OPEN INTERMITTENTLY BY RECONNECTION. SOLAR EJECTA SHARE CHARACTERISTICS WITH SLOW WINDS AND MAY ORIGINATE FROM SIMILAR SOURCE REGIONS. THIS PROJECT WILL INVESTIGATE THE TURBULENCE IN THE SLOW SOLAR WIND AND SOLAR EJECTA USING A THREE-DIMENSIONAL HYBRID KINETIC SIMULATION. A HYBRID NUMERICAL MODEL WILL BE EMPLOYED WITH PARTICLE IONS AND FLUID ELECTRONS. TURBULENCE WILL BE DIRECTLY COMPUTED AND SPECIFICS OF THE NATURE OF THE ION KINETIC PROCESSES AND FLUCTUATIONS AT THE ION KINETIC SCALES WILL BE OBTAINED. THERE ARE THREE PROJECT GOALS. THE FIRST GOAL IS TO IDENTIFY THE NATURE OF TURBULENT FLUCTUATIONS IN SLOW WINDS AND EJECTA. WAVE-MODES AND COHERENT STRUCTURES WILL BE SOUGHT IN SIMULATION RESULTS. COMPARISON OF SIMULATION RESULTS AND OBSERVATIONS WILL ALSO BE MADE. ANOTHER GOAL IS TO DETERMINE THE ION HEATING PROCESSES THAT OPERATE IN SLOW WINDS AND EJECTA. ION PARTICLE TRACKING WILL BE USED IN SIMULATIONS TO DETAIL THE NATURE OF STOCHASTIC ION MOTIONS AND RELATE THESE MOTIONS TO PROCESSES INVOLVING THE DISSIPATION OF FLUCTUATIONS AND THE NET GAIN OF ION THERMAL ENERGY. THE LAST GOAL IS TO DETERMINE THE PARTITION OF ION HEATING IN SLOW WINDS AND EJECTA BETWEEN HELIUM AND HYDROGEN. SIMULATIONS WILL BE CONDUCTED WITH THE VARIABLE HELIUM TO HYDROGEN DENSITY RATIOS FOUND IN THE SLOW WINDS AND EJECTA. PUBLICLY AVAILABLE WIND SPACECRAFT MAGNETIC FIELD AND PLASMA DATA FROM SLOW WINDS AND SOLAR EJECTA WILL BE USED TO EXAMINE THE NATURE OF FLUCTUATIONS AND COMPARE WITH ION HEATING RATES. THE PROPERTIES OF TURBULENT FLUCTUATIONS IN VARIOUS CLASSES OF SOLAR EJECTA WILL ALSO BE STUDIED. THIS PROPOSAL ADDRESSES THE PROBLEM OF COUPLING OF SMALL-SCALE PROCESSES IN THE SOLAR WIND TO ITS LARGE-SCALE DYNAMICS THROUGH A TURBULENT ENERGY CASCADE. NEW QUANTITATIVE INFORMATION ABOUT THE PROPERTIES OF INTERPLANETARY TURBULENCE IS RELEVANT TO THE DECADAL SURVEY GOAL TO "DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE." THE PROPOSED WORK WILL ALSO FURTHER THE GOALS OF THE WIND SPACECRAFT MISSION TO INVESTIGATE AND CHARACTERIZE THE FUNDAMENTAL PLASMA PROCESSES THAT TAKE PLACE NEAR 1 AU AND THE EVOLUTION OF SOLAR EJECTA.