ANALYZING GENESIS SOLAR WIND SAMPLES BY ION MICROPROBE. THE GENESIS MISSION WAS CARRIED OUT TO RETURN A SAMPLE OF THE SOLAR WIND TO EARTH IN ORDER TO OBTAIN PRECISE ISOTOPIC COMPOSITIONS AND ABUNDANCES OF THE ELEMENTS IN THE SOLAR WIND. OUR LABORATORY HAS BEEN ANALYZING GENESIS SAMPLES FOR SEVERAL YEARS AND WE HAVE DEVELOPED STATE-OF-THE-ART TECHNIQUES TO OBTAIN HIGH-PRECISION ISOTOPIC AND ELEMENTAL COMPOSITIONS. WE COLLECT BACK-SIDE DEPTH PROFILES IN IMAGE MODE USING RASTER ION IMAGING TO COLLECTED IMAGE STACKS THAT WE CAN THEN PROCESS. EACH PIXEL IN THE IMAGE IS A DEPTH PROFILE. WE ALIGN THE STACK IN X AND Y TO ACCOUNT FOR BEAM DRIFT. THEN WE ALIGN THE PIXELS IN THE IMAGE SO THAT THE PEAK OF THE SOLAR WIND AND THE BREAKTHROUGH AT THE SURFACE ARE AT THE SAME DEPTH IN ALL PIXELS. WE THEN COMBINE THE PIXELS TO PRODUCE THE FINAL DEPTH PROFILE FOR THAT MEASUREMENT. WE HAVE ALSO LEARNED HOW TO RELIABLY STANDARDIZE THE MEASUREMENTS. WE PROPOSE TO LEVERAGE WHAT WE HAVE LEARNED TO MAKE MEASUREMENTS OF THE FLUENCES AND ISOTOPIC COMPOSITIONS OF A VARIETY OF ELEMENTS IN THE GENESIS COLLECTORS. USING A CS PRIMARY BEAM WE WILL MEASURE C O AND S IN SI COLLECTORS AND SI IN SAPPHIRE COLLECTORS. USING AN O PRIMARY ION BEAM WE WILL MEASURE AL CA CR AND FE IN SI COLLECTORS AND NA IN EITHER DOS OR SAPPHIRE COLLECTORS. TECHNIQUES WILL HAVE TO BE DEVELOPED TO WORK THE THE SAPPHIRE COLLECTORS BUT OUR PRELIMINARY WORK SHOWS HOW THIS CAN BE DONE. SAMPLE PREPARATION WILL BE DONE AT BERKELEY STANDARDIZATION WILL BE DONE COLLABORATIVELY BETWEEN BERKELEY UH FSU ASU AND CALTECH THE MEASUREMENTS WILL BE DONE AT UH PIT DEPTHS WILL BE MEASURED AT ASU AND THE DATA REDUCTION WILL BE DONE AT UH WITH INPUT FROM BERKELEY AND WASH. U. PAPERS REPORTING THE DATA WILL BE WRITTEN AT UH ALTHOUGH THE ENTIRE TEAM WILL HAVE INPUT INTO THE FINAL DOCUMENT. THIS WORK WILL HELP MAXIMIZE THE SCIENTIFIC RETURN OF THE GENESIS MISSION THOUGH DIRECT ANALYSIS OF SAMPLES THAT GENESIS RETURNED TO EARTH. THE GENESIS MISSION IS EXPLICITLY CALLED OUT IN THE REQUEST FOR PROPOSALS AS ONE OF THE TARGETS FOR THE LARS PROGRAM (C.18 2.1.1). ACCOMPANYING THIS PROPOSAL IS A PLANETARY MAJOR EQUIPMENT REQUEST TO OBTAIN A NEW RF PLASMA OXYGEN ION SOURCE FOR THE CAMECA IMS 1280 ION MICROPROBE. THIS SOURCE WOULD GREATLY FACILITATE THE WORK ON ELEMENTS THAT MAKE POSITIVE IONS (NA AL CA CR TI FE MN NI ETC) BY PROVIDING MUCH GREATER LONG TERM STABILITY (CLEANING UP OUR DEPTH PROFILES) AND A MUCH SMALLER SPOT SIZE (DE-SMEARING OUR DEPTH PROFILES). IF WE DO NOT GET THE SOURCE THE WORK CAN AND WILL STILL BE DONE BUT THE UNCERTAINTIES WILL BE LARGER