OBJECTIVES: I PROPOSE A DATA ANALYSIS PROGRAM TO PERFORM THE FIRST GLOBAL CHARACTERIZATION OF TURBULENCE IN THE PLASMA ENVIRONMENT OF COMET 67P. I WILL USE THE ROSETTA SPACECRAFT'S MAGNETOMETER MEASUREMENTS TO PERFORM THIS TASK. INTRODUCTION: TURBULENCE REFERS TO FLUCTUATIONS AND THEIR NONLINEAR INTERACTIONS ARISING IN FLUIDS AND PLASMAS. FOR FLUIDS TURBULENCE CAN ARISE IN FLUID QUANTITIES SUCH AS THE FLUID FLOW VELOCITY AND FOR MAGNETIZED PLASMAS TURBULENCE CAN ARISE IN THE MAGNETIC FIELD AND PLASMA FLOW VELOCITY. INVESTIGATIONS OF TURBULENCE ENABLE TO REVEAL HOW ENERGY INJECTED AT LARGE SCALES IS TRANSFERRED TO SMALL SCALES AND ULTIMATELY TO PARTICLE HEATING. IN THE HYDRODYNAMIC ANALOG OF A COFFEE CUP ENERGY INJECTED BY STIRRING THE COFFEE FIRST GENERATES EDDIES WITH A SIZE OF THE DIAMETER OF THE COFFEE CUP. THESE EDDIES THEN NONLINEARLY INTERACT WITH ONE ANOTHER TO CREATE MUCH SMALLER EDDIES AND TRANSFER THE ENERGY TO SMALLER SCALES IN A PROCESS KNOWN AS THE ENERGY CASCADE. WHEN THE EDDY SIZES BECOME COMPARABLE TO THE VISCOUS SCALES OF THE FLUID THE ENERGY IS TRANSFERRED TO PARTICLE HEATING. INVESTIGATIONS OF TURBULENCE IN THE SOLAR WIND AND PLANETARY PLASMA ENVIRONMENTS HAVE REVEALED THAT TURBULENCE EVOLVES IN THESE ENVIRONMENTS IN A MANNER SIMILAR TO THE HYDRODYNAMIC ANALOG OF THE COFFEE CUP. IN THESE PLASMA ENVIRONMENTS WAVES EXCITED AT LOW FREQUENCIES OR AT LARGE WAVELENGTHS NONLINEARLY INTERACT WITH ONE ANOTHER JUST LIKE THE EDDIES IN A COFFEE CUP AND TRANSFER THE ENERGY TO HIGHER FREQUENCIES OR SMALLER WAVELENGTHS ULTIMATELY LEADING TO PARTICLE HEATING. IN MY PROPOSED WORK I WILL USE THE PLASMA ENVIRONMENT OF COMET 67P AS A LABORATORY FOR STUDYING TURBULENCE. WHILE TURBULENCE HAS BEEN STUDIED AT COMETS PREVIOUSLY THESE STUDIES WERE LIMITED BY THE SHORT OBSERVATION DURATIONS OF THE FLYBY MISSIONS. ROSETTA SPACECRAFT ON THE OTHER HAND MADE COMPREHENSIVE OBSERVATIONS AT COMET 67P FOR OVER A YEAR AND THE OBSERVATIONS ALSO COVERED A LARGE SPATIAL REGION SURROUNDING THE COMET. THESE LONG OBSERVATION TIMES AND THE COMPREHENSIVE SPATIAL COVERAGE ARE IDEAL FOR STUDYING THE TEMPORAL AND SPATIAL EVOLUTION OF TURBULENCE AT A COMET. MOREOVER THE ROSETTA OBSERVATIONS WERE CONDUCTED ON A TIME FRAME CENTERED ON THE COMET'S PERIHELION AND THIS IS ALSO IDEAL FOR STUDYING HOW CHANGING COMET-SUN DISTANCES HENCE ITS OUTGASSING ACTIVITY INFLUENCES THE EVOLUTION OF TURBULENCE. COMET 67P WAS ALSO FOUND TO BE A WEAKLY OUTGASSING COMET THUS THIS INVESTIGATION WILL ALSO ENABLE COMPARISON OF TURBULENCE AT WEAK VS. STRONG OUTGASSING COMETS (SUCH AS HALLEY). IN MY INVESTIGATION I WILL SEEK ANSWERS TO THE FOLLOWING QUESTIONS: 1. WHERE AND WHEN IN THE PLASMA ENVIRONMENT OF COMET 67P ARE TURBULENT PROCESSES SUCH AS ENERGY INJECTION CASCADE AND HEATING PRESENT? 2. HOW DO THESE TURBULENT PROCESSES EVOLVE WITH DIFFERENT COMET-SUN DISTANCES? 3. HOW DO THE TURBULENT PROCESSES OBSERVED AT COMET 67P COMPARE TO TURBULENT PROCESSES OBSERVED AT OTHER COMETS AND PLANETARY PLASMA ENVIRONMENTS? METHOD: TO CONDUCT THE PROPOSED STUDY I WILL ANALYZE MAGNETOMETER DATA FROM THE ROSETTA SPACE PROBE. I WILL COMPUTE POWER SPECTRA OF MAGNETIC FIELD FLUCTUATIONS FROM THE MAGNETIC FIELD TIME SERIES MEASURED BY THE ROSETTA MAGNETOMETER. THEN I WILL DETERMINE THE SLOPES IN THESE POWER SPECTRA WHICH HAVE DIFFERENT VALUES FOR ENERGY INJECTION ENERGY CASCADE AND HEATING ENABLING THEIR IDENTIFICATION AT COMET 67P. I WILL DETERMINE HOW THESE POWER SPECTRA SLOPE VALUES CHANGE IN THE SPACE SURROUNDING THE COMET 67P AND WITH DIFFERENT COMET-SUN DISTANCES TO REVEAL THE PROCESSES THAT BECOME DOMINANT IN DIFFERENT SPATIAL REGIONS AND TIMES. BY COMPARISON OF THE POWER SPECTRA SLOPE VALUES OBSERVED AT COMET 67P WITH THOSE OBSERVED AT OTHER COMETS AND PLANETARY PLASMA ENVIRONMENTS I WILL DETERMINE HOW TURBULENT PROCESSES OBSERVED AT COMET 67P ARE SIMILAR TO AND DIFFERENT FROM THE PROCESSES OBSERVED AT THOSE PLASMA ENVIRONMENTS.