4 WE PROPOSE TO OBTAIN HIGH PRECISION OXYGEN AND MAGNESIUM ISOTOPE ANALYSES OF PARTICLES RECOVERED FROM THE COMET 81P WILD 2 STARDUST MISSION USING A SECONDARY ION MASS SPECTROMETER IMS 1280 AT UNIVERSITY OF WISCONSIN WISCSIMS IN ORDER TO UNDERSTAND THE ORIGIN OF THE PARTICLES IN THE EARLY SOLAR SYSTEM. A RELATIONSHIP BETWEEN OXYGEN ISOTOPE RATIOS AND MG MOLAR MGO MGO FE OF OLIVINE AND PYROXENE IS INDICATIVE TO THEIR FORMATION ENVIRONMENTS AND ISOTOPE RESERVOIRS AND PROVIDE A CLUE TO THE LOCATION WHERE THEY FORMED IN THE PROTOPLANSTARY DISK. MAGNESIUM ISOTOPES PROVIDE CHRONOLOGY OF PARTICLES THROUGH THE DECAY OF 26A TO DAUGHTER 26MG HALF LIFE OF 0.7 MILLION YEARS AND OR EVIDENCE OF HIGH TEMPERATURE PROCESSES BETWEEN SOLID AND GAS EVAPORATION AND CONDENSATION AS STABLE ISOTOPE FRACTIONATION. DETAILED ISOTOPE STUDIES COMBINED WITH MINERALOGY AND CHEMISTRY WILL BE A KEY TO UNDERSTAND HOW THESE HIGH TEMPERATURE PARTICLES FORMED AND WERE TRANSPORTED TO COMET FORMING REGIONS. WE PLAN TO ANALYZE RELATIVELY LARGER A FEW M CRYSTALLINE SILICATES USING 2 M SIMS SPOT SIZE. PARTICLES ARE SELECTED ACCORDING TO THE MINERALOGY AND MAJOR ELEMENT CHEMISTRY THAT ARE OBTAINED FROM THE MICROTOME TEM SECTIONS BY COLLABORATORS U. WASHINGTON AND NASA JSC. WE FOCUS ON HIGH MG OLIVINE AND PYROXENE, WHICH ARE KNOWN TO BE EITHER CHONDRULE LIKE OBJECTS OR CONDENSATES OF THE EARLY SOLAR SYSTEM, SUCH AS LIME LOW IRON, MANGANESE ENRICHED OLIVINE. MAGNESIUM ISOTOPE ANALYSES WILL BE PERFORMED ALL PARTICLES THAT SHOW 16O RICH ISOTOPE SIGNATURES AND THOSE CONTAINING AL RICH PHASES LARGER THAN 3 M IN SIZE. WE PROPOSE TO ACQUIRE NEW OXYGEN PRIMARY ION SOURCE OF THE IMS 1280 RF PLASMA SOURCE THAT WILL PROVIDE HIGHER PRIMARY BEAM INTENSITY FOR SMALL SPOT SIZES AT LEAST 10 TIMES OR EVEN HIGHER THAN THAT OF CURRENT ION SOURCE. THE HIGHER PRIMARY BEAM INTENSITY WILL IMPROVE SECONDARY ION INTENSITIES, WHICH RESULTS IN IMPROVEMENTS IN ANALYTICAL PRECISIONS. RESULTS OBTAINED FROM THE PROPOSED STUDIES WILL MAXIMIZE SCIENTIFIC RETURN FROM THE SAMPLES PROVIDED BY STARDUST MISSION AND ADVANCE OUR KNOWLEDGE OF THE EARLY EVOLUTION OF SOLAR SYSTEM, WHICH COULD NOT BE OBTAINED SOLELY FROM STUDIES OF PRIMITIVE METEORITES. ANALYTICAL TECHNIQUES ESTABLISHED IN THE PROPOSED RESEARCH WILL BENEFIT THE ANALYSIS OF METEORITES, INTERPLANETARY DUST PARTICLES, AND SAMPLES FROM FUTURE PLANETARY RETURN MISSIONS. Other Administrative Action $0 2/7/19 Not listed WE PROPOSE TO OBTAIN HIGH PRECISION OXYGEN AND MAGNESIUM ISOTOPE ANALYSES OF PARTICLES RECOVERED FROM THE COMET 81P WILD 2 STARDUST MISSION USING A SECONDARY ION MASS SPECTROMETER IMS 1280 AT UNIVERSITY OF WISCONSIN WISCSIMS IN ORDER TO UNDERSTAND THE ORIGIN OF THE PARTICLES IN THE EARLY SOLAR SYSTEM. A RELATIONSHIP BETWEEN OXYGEN ISOTOPE RATIOS AND MG MOLAR MGO MGO FE OF OLIVINE AND PYROXENE IS INDICATIVE TO THEIR FORMATION ENVIRONMENTS AND ISOTOPE RESERVOIRS AND PROVIDE A CLUE TO THE LOCATION WHERE THEY FORMED IN THE PROTOPLANSTARY DISK. MAGNESIUM ISOTOPES PROVIDE CHRONOLOGY OF PARTICLES THROUGH THE DECAY OF 26A TODAUGHTER 26MG HALF LIFE OF 0.7 MILLION YEARS AND OR EVIDENCE OF HIGH TEMPERATURE PROCESSES BETWEEN SOLID AND GAS EVAPORATION AND CONDENSATION AS STABLE ISOTOPE FRACTIONATION. DETAILED ISOTOPE STUDIES COMBINED WITH MINERALOGY AND CHEMISTRY WILL BE A KEY TO UNDERSTAND HOW THESE HIGH TEMPERATURE PARTICLES FORMED AND WERE TRANSPORTED TO COMET FORMING REGIONS.WE PLAN TO ANALYZE RELATIVELY LARGER A FEW M CRYSTALLINE SILICATES USING 2 M SIMS SPOT SIZE. PARTICLES ARE SELECTED ACCORDING TO THE MINERALOGY AND MAJOR ELEMENT CHEMISTRY THAT ARE OBTAINED FROM THE MICROTOME TEM SECTIONS BY COLLABORATORS U. WASHINGTON AND NASA JSC. WE FOCUS ON HIGH MG OLIVINE AND PYROXENE WHICH ARE KNOWN TO BE EITHER CHONDRULE LIKE OBJECTS OR CONDENSATES OF THE EARLY SOLAR SYSTEM SUCH AS LIME LOW IRON MANGANESE ENRICHED OLIVINE. MAGNESIUM ISOTOPE ANALYSES WILL BE PERFORMED ALL PARTICLES THAT SHOW 16O RICH ISOTOPE SIGNATURES AND THOSE CONTAINING AL RICH PHASES LARGER THAN 3 M IN SIZE.WE PROPOSE TO ACQUIRE NEW OXYGEN PRIMARY ION SOURCE OF THE IMS 1280 RF PLASMA SOURCE THAT WILL PROVIDE HIGHER PRIMARY BEAM INTENSITY FOR SMALL SPOT SIZES AT LEAST 10 TIMES OR EVEN HIGHER THAN THAT OF CURRENT ION SOURCE. THE HIGHER PRIMARY BEAM INTENSITY WILL IMPROVE SECONDARY ION INTENSITIES WHICH RESULTS IN IMPROVEMENTS IN ANALYTICAL PRECISIONS.RESULTS OBTAINED FROM THE PROPOSED STUDIES WILL MAXIMIZE SCIENTIFIC RETURN FROM THE SAMPLES PROVIDED BY STARDUST MISSION AND ADVANCE OUR KNOWLEDGE OF THE EARLY EVOLUTION OF SOLAR SYSTEM WHICH COULD NOT BE OBTAINED SOLELY FROM STUDIES OF PRIMITIVE METEORITES. ANALYTICAL TECHNIQUES ESTABLISHED IN THE PROPOSED RESEARCH WILL BENEFIT THE ANALYSIS OF METEORITES INTERPLANETARY DUST PARTICLES ANDSAMPLES FROM FUTURE PLANETARY RETURN MISSIONS. $0 2/7/19 3 WE PROPOSE TO OBTAIN HIGH PRECISION OXYGEN AND MAGNESIUM ISOTOPE ANALYSES OF PARTICLES RECOVERED FROM THE COMET 81P WILD 2 STARDUST MISSION USING A SECONDARY ION MASS SPECTROMETER IMS 1280 AT UNIVERSITY OF WISCONSIN WISCSIMS IN ORDER TO UNDERSTAND THE ORIGIN OF THE PARTICLES IN THE EARLY SOLAR SYSTEM. A RELATIONSHIP BETWEEN OXYGEN ISOTOPE RATIOS AND MG MOLAR MGO MGO FE OF OLIVINE AND PYROXENE IS INDICATIVE TO THEIR FORMATION ENVIRONMENTS AND ISOTOPE RESERVOIRS AND PROVIDE A CLUE TO THE LOCATION WHERE THEY FORMED IN THE PROTOPLANSTARY DISK. MAGNESIUM ISOTOPES PROVIDE CHRONOLOGY OF PARTICLES THROUGH THE DECAY OF 26A TO DAUGHTER 26MG HALF LIFE OF 0.7 MILLION YEARS AND OR EVIDENCE OF HIGH TEMPERATURE PROCESSES BETWEEN SOLID AND GAS EVAPORATION AND CONDENSATION AS STABLE ISOTOPE FRACTIONATION. DETAILED ISOTOPE STUDIES COMBINED WITH MINERALOGY AND CHEMISTRY WILL BE A KEY TO UNDERSTAND HOW THESE HIGH TEMPERATURE PARTICLES FORMED AND WERE TRANSPORTED TO COMET FORMING REGIONS. WE PLAN TO ANALYZE RELATIVELY LARGER A FEW M CRYSTALLINE SILICATES USING 2 M SIMS SPOT SIZE. PARTICLES ARE SELECTED ACCORDING TO THE MINERALOGY AND MAJOR ELEMENT CHEMISTRY THAT ARE OBTAINED FROM THE MICROTOME TEM SECTIONS BY COLLABORATORS U. WASHINGTON AND NASA JSC. WE FOCUS ON HIGH MG OLIVINE AND PYROXENE, WHICH ARE KNOWN TO BE EITHER CHONDRULE LIKE OBJECTS OR CONDENSATES OF THE EARLY SOLAR SYSTEM, SUCH AS LIME LOW IRON, MANGANESE ENRICHED OLIVINE. MAGNESIUM ISOTOPE ANALYSES WILL BE PERFORMED ALL PARTICLES THAT SHOW 16O RICH ISOTOPE SIGNATURES AND THOSE CONTAINING AL RICH PHASES LARGER THAN 3 M IN SIZE. WE PROPOSE TO ACQUIRE NEW OXYGEN PRIMARY ION SOURCE OF THE IMS 1280 RF PLASMA SOURCE THAT WILL PROVIDE HIGHER PRIMARY BEAM INTENSITY FOR SMALL SPOT SIZES AT LEAST 10 TIMES OR EVEN HIGHER THAN THAT OF CURRENT ION SOURCE. THE HIGHER PRIMARY BEAM INTENSITY WILL IMPROVE SECONDARY ION INTENSITIES, WHICH RESULTS IN IMPROVEMENTS IN ANALYTICAL PRECISIONS. RESULTS OBTAINED FROM THE PROPOSED STUDIES WILL MAXIMIZE SCIENTIFIC RETURN FROM THE SAMPLES PROVIDED BY STARDUST MISSION AND ADVANCE OUR KNOWLEDGE OF THE EARLY EVOLUTION OF SOLAR SYSTEM, WHICH COULD NOT BE OBTAINED SOLELY FROM STUDIES OF PRIMITIVE METEORITES. ANALYTICAL TECHNIQUES ESTABLISHED IN THE PROPOSED RESEARCH WILL BENEFIT THE ANALYSIS OF METEORITES, INTERPLANETARY DUST PARTICLES, AND SAMPLES FROM FUTURE PLANETARY RETURN MISSIONS. Funding Only Action $73.2k 8/16/18 Not listed WE PROPOSE TO OBTAIN HIGH PRECISION OXYGEN AND MAGNESIUM ISOTOPE ANALYSES OF PARTICLES RECOVERED FROM THE COMET 81P WILD 2 STARDUST MISSION USING A SECONDARY ION MASS SPECTROMETER IMS 1280 AT UNIVERSITY OF WISCONSIN WISCSIMS IN ORDER TO UNDERSTAND THE ORIGIN OF THE PARTICLES IN THE EARLY SOLAR SYSTEM. A RELATIONSHIP BETWEEN OXYGEN ISOTOPE RATIOS AND MG MOLAR MGO MGO FE OF OLIVINE AND PYROXENE IS INDICATIVE TO THEIR FORMATION ENVIRONMENTS AND ISOTOPE RESERVOIRS AND PROVIDE A CLUE TO THE LOCATION WHERE THEY FORMED IN THE PROTOPLANSTARY DISK. MAGNESIUM ISOTOPES PROVIDE CHRONOLOGY OF PARTICLES THROUGH THE DECAY OF 26A TODAUGHTER 26MG HALF LIFE OF 0.7 MILLION YEARS AND OR EVIDENCE OF HIGH TEMPERATURE PROCESSES BETWEEN SOLID AND GAS EVAPORATION AND CONDENSATION AS STABLE ISOTOPE FRACTIONATION. DETAILED ISOTOPE STUDIES COMBINED WITH MINERALOGY AND CHEMISTRY WILL BE A KEY TO UNDERSTAND HOW THESE HIGH TEMPERATURE PARTICLES FORMED AND WERE TRANSPORTED TO COMET FORMING REGIONS.WE PLAN TO ANALYZE RELATIVELY LARGER A FEW M CRYSTALLINE SILICATES USING 2 M SIMS SPOT SIZE. PARTICLES ARE SELECTED ACCORDING TO THE MINERALOGY AND MAJOR ELEMENT CHEMISTRY THAT ARE OBTAINED FROM THE MICROTOME TEM SECTIONS BY COLLABORATORS U. WASHINGTON AND NASA JSC. WE FOCUS ON HIGH MG OLIVINE AND PYROXENE WHICH ARE KNOWN TO BE EITHER CHONDRULE LIKE OBJECTS OR CONDENSATES OF THE EARLY SOLAR SYSTEM SUCH AS LIME LOW IRON MANGANESE ENRICHED OLIVINE. MAGNESIUM ISOTOPE ANALYSES WILL BE PERFORMED ALL PARTICLES THAT SHOW 16O RICH ISOTOPE SIGNATURES AND THOSE CONTAINING AL RICH PHASES LARGER THAN 3 M IN SIZE.WE PROPOSE TO ACQUIRE NEW OXYGEN PRIMARY ION SOURCE OF THE IMS 1280 RF PLASMA SOURCE THAT WILL PROVIDE HIGHER PRIMARY BEAM INTENSITY FOR SMALL SPOT SIZES AT LEAST 10 TIMES OR EVEN HIGHER THAN THAT OF CURRENT ION SOURCE. THE HIGHER PRIMARY BEAM INTENSITY WILL IMPROVE SECONDARY ION INTENSITIES WHICH RESULTS IN IMPROVEMENTS IN ANALYTICAL PRECISIONS.RESULTS OBTAINED FROM THE PROPOSED STUDIES WILL MAXIMIZE SCIENTIFIC RETURN FROM THE SAMPLES PROVIDED BY STARDUST MISSION AND ADVANCE OUR KNOWLEDGE OF THE EARLY EVOLUTION OF SOLAR SYSTEM WHICH COULD NOT BE OBTAINED SOLELY FROM STUDIES OF PRIMITIVE METEORITES. ANALYTICAL TECHNIQUES ESTABLISHED IN THE PROPOSED RESEARCH WILL BENEFIT THE ANALYSIS OF METEORITES INTERPLANETARY DUST PARTICLES ANDSAMPLES FROM FUTURE PLANETARY RETURN MISSIONS. $73.2k 8/16/18 2 WE PROPOSE TO OBTAIN HIGH PRECISION OXYGEN AND MAGNESIUM ISOTOPE ANALYSES OF PARTICLES RECOVERED FROM THE COMET 81P WILD 2 STARDUST MISSION USING A SECONDARY ION MASS SPECTROMETER IMS 1280 AT UNIVERSITY OF WISCONSIN WISCSIMS IN ORDER TO UNDERSTAND THE ORIGIN OF THE PARTICLES IN THE EARLY SOLAR SYSTEM. A RELATIONSHIP BETWEEN OXYGEN ISOTOPE RATIOS AND MG MOLAR MGO MGO FE OF OLIVINE AND PYROXENE IS INDICATIVE TO THEIR FORMATION ENVIRONMENTS AND ISOTOPE RESERVOIRS AND PROVIDE A CLUE TO THE LOCATION WHERE THEY FORMED IN THE PROTOPLANSTARY DISK. MAGNESIUM ISOTOPES PROVIDE CHRONOLOGY OF PARTICLES THROUGH THE DECAY OF 26A TO DAUGHTER 26MG HALF LIFE OF 0.7 MILLION YEARS AND OR EVIDENCE OF HIGH TEMPERATURE PROCESSES BETWEEN SOLID AND GAS EVAPORATION AND CONDENSATION AS STABLE ISOTOPE FRACTIONATION. DETAILED ISOTOPE STUDIES COMBINED WITH MINERALOGY AND CHEMISTRY WILL BE A KEY TO UNDERSTAND HOW THESE HIGH TEMPERATURE PARTICLES FORMED AND WERE TRANSPORTED TO COMET FORMING REGIONS. WE PLAN TO ANALYZE RELATIVELY LARGER A FEW M CRYSTALLINE SILICATES USING 2 M SIMS SPOT SIZE. PARTICLES ARE SELECTED ACCORDING TO THE MINERALOGY AND MAJOR ELEMENT CHEMISTRY THAT ARE OBTAINED FROM THE MICROTOME TEM SECTIONS BY COLLABORATORS U. WASHINGTON AND NASA JSC. WE FOCUS ON HIGH MG OLIVINE AND PYROXENE, WHICH ARE KNOWN TO BE EITHER CHONDRULE LIKE OBJECTS OR CONDENSATES OF THE EARLY SOLAR SYSTEM, SUCH AS LIME LOW IRON, MANGANESE ENRICHED OLIVINE. MAGNESIUM ISOTOPE ANALYSES WILL BE PERFORMED ALL PARTICLES THAT SHOW 16O RICH ISOTOPE SIGNATURES AND THOSE CONTAINING AL RICH PHASES LARGER THAN 3 M IN SIZE. WE PROPOSE TO ACQUIRE NEW OXYGEN PRIMARY ION SOURCE OF THE IMS 1280 RF PLASMA SOURCE THAT WILL PROVIDE HIGHER PRIMARY BEAM INTENSITY FOR SMALL SPOT SIZES AT LEAST 10 TIMES OR EVEN HIGHER THAN THAT OF CURRENT ION SOURCE. THE HIGHER PRIMARY BEAM INTENSITY WILL IMPROVE SECONDARY ION INTENSITIES, WHICH RESULTS IN IMPROVEMENTS IN ANALYTICAL PRECISIONS. RESULTS OBTAINED FROM THE PROPOSED STUDIES WILL MAXIMIZE SCIENTIFIC RETURN FROM THE SAMPLES PROVIDED BY STARDUST MISSION AND ADVANCE OUR KNOWLEDGE OF THE EARLY EVOLUTION OF SOLAR SYSTEM, WHICH COULD NOT BE OBTAINED SOLELY FROM STUDIES OF PRIMITIVE METEORITES. ANALYTICAL TECHNIQUES ESTABLISHED IN THE PROPOSED RESEARCH WILL BENEFIT THE ANALYSIS OF METEORITES, INTERPLANETARY DUST PARTICLES, AND SAMPLES FROM FUTURE PLANETARY RETURN MISSIONS. Funding Only Action $42.8k 9/22/17