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Paque JM, Hofmann AE, Burnett DS, Guan Y, Jurewicz AJG, Woolum DS, Ma C, Rossman GR. Electron Microprobe/SIMS Determinations of Al in Olivine: Applications to Solar Wind, Pallasites and Trace Element Measurements. Geostand Geoanal Res 2020; 44:473-484. [PMID: 34381324 PMCID: PMC8350971 DOI: 10.1111/ggr.12347] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Electron probe microanalyzer measurements of trace elements with high accuracy are challenging. Accurate Al measurements in olivine are required to calibrate SIMS implant reference materials for measurement of Al in the solar wind. We adopt a combined EPMA/SIMS approach that is useful for producing SIMS reference materials as well as for EPMA at the ~100 μg g-1 level. Even for mounts not polished with alumina photoelectron spectroscopy shows high levels of Al surface contamination. In order to minimize electron beam current density, a rastered 50 × 100 μm electron beam was adequate and minimized sensitivity to small Al-rich contaminants. Reproducible analyses of eleven SIMS-cleaned spots on San Carlos olivine agreed at 69.3 ± 1.0 μg g-1• The known Al mass fraction was used to calibrate an Al implant into San Carlos. Accurate measurements of Al were made for olivines in the pallasites: lmilac, Eagle Station and Springwater. Our focus was on Al in olivine, but our technique could be refined to give accurate electron probe measurements for other contamination-sensitive trace elements. For solar wind, it is projected that the Al/Mg abundance ratio can be determined to 6%, a factor of 2 more precise than the solar spectroscopic ratio.
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Affiliation(s)
- J M Paque
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
| | - A E Hofmann
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91107
| | - D S Burnett
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
| | - Y Guan
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
| | | | - D S Woolum
- Dept. of Physics, Cal State Fullerton, Fullerton CA 92834
| | - C Ma
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
| | - G R Rossman
- California Institute of Technology, Div. of Geol. and Planet. Sciences, Pasadena, CA 91104
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Jurewicz AJG, Rieck KD, Hervig R, Burnett DS, Wadhwa M, Olinger CT, Wiens RC, Laming JM, Guan Y, Huss GR, Reisenfeld DB, Williams P. Magnesium isotopes of the bulk solar wind from Genesis diamond-like carbon films. Meteorit Planet Sci 2020; 55:352-375. [PMID: 32214784 PMCID: PMC7079557 DOI: 10.1111/maps.13439] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/09/2018] [Accepted: 12/10/2019] [Indexed: 06/10/2023]
Abstract
NASA's Genesis Mission returned solar wind (SW) to the Earth for analysis to derive the composition of the solar photosphere from solar material. SW analyses control the precision of the derived solar compositions, but their ultimate accuracy is limited by the theoretical or empirical models of fractionation due to SW formation. Mg isotopes are "ground truth" for these models since, except for CAIs, planetary materials have a uniform Mg isotopic composition (within ≤1‰) so any significant isotopic fractionation of SW Mg is primarily that of SW formation and subsequent acceleration through the corona. This study analyzed Mg isotopes in a bulk SW diamond-like carbon (DLC) film on silicon collector returned by the Genesis Mission. A novel data reduction technique was required to account for variable ion yield and instrumental mass fractionation (IMF) in the DLC. The resulting SW Mg fractionation relative to the DSM-3 laboratory standard was (-14.4‰, -30.2‰) ± (4.1‰, 5.5‰), where the uncertainty is 2ơ SE of the data combined with a 2.5‰ (total) error in the IMF determination. Two of the SW fractionation models considered generally agreed with our data. Their possible ramifications are discussed for O isotopes based on the CAI nebular composition of McKeegan et al. (2011).
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Affiliation(s)
- A. J. G. Jurewicz
- Center for Meteorite StudiesArizona State Universitym/c 6004TempeArizona85287USA
| | - K. D. Rieck
- New Mexico Consortium4200 West Jemez Road Suite 200Los AlamosNew Mexico87544USA
| | - R. Hervig
- School of Earth and Space ExplorationArizona State UniversityTempeArizona85287USA
| | - D. S. Burnett
- Department of Geology and Planetary SciencesCalifornia Institute of Technologym/c 100‐23PasadenaCalifornia91125USA
| | - M. Wadhwa
- School of Earth and Space ExplorationArizona State UniversityTempeArizona85287USA
| | - C. T. Olinger
- GET‐NSA, LLC, AU‐6219901 Germantown RdGermantownMaryland20875USA
| | - R. C. Wiens
- Los Alamos National Laboratory (Remote Sensing)ISR‐2, m/s C‐331Los AlamosNew Mexico87545USA
| | - J. M. Laming
- Naval Research LaboratorySpace Science DivisionCode 7684WashingtonDistrict of Columbia20375USA
| | - Y. Guan
- Geological and Planetary SciencesCalifornia Institute of Technologym/c 100‐10PasadenaCalifornia91125USA
| | - G. R. Huss
- Hawaii Institute of Geophysics and PlanetologyUniversity of Hawaii at Manoa1680 East‐West Road, Post 504HonoluluHawaii96822USA
| | - D. B. Reisenfeld
- Los Alamos National Laboratory ISR‐1Los AlamosNew Mexico87545USA
| | - P. Williams
- School of Molecular SciencesArizona State UniversityTempeArizona85287USA
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Burnett DS, Jurewicz AJG, Woolum DS. The future of Genesis science. Meteorit Planet Sci 2019; 54:1092-1114. [PMID: 31130804 PMCID: PMC6519397 DOI: 10.1111/maps.13266] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 09/07/2016] [Accepted: 01/30/2019] [Indexed: 06/09/2023]
Abstract
Solar abundances are important to planetary science since the prevalent model assumes that the composition of the solar photosphere is that of the solar nebula from which planetary materials formed. Thus, solar abundances are a baseline for planetary science. Previously, solar abundances have only been available through spectroscopy or by proxy (CI). The Genesis spacecraft collected and returned samples of the solar wind for laboratory analyses. Elemental and isotopic abundances in solar wind from Genesis samples have been successfully measured despite the crash of the re-entry capsule. Here we present science rationales for a set of 12 important (and feasible postcrash) Science and Measurement Objectives as goals for the future (Table 1). We also review progress in Genesis sample analyses since the last major review (Burnett 2013). Considerable progress has been made toward understanding elemental fractionation during the extraction of the solar wind from the photosphere, a necessary step in determining true solar abundances from solar wind composition. The suitability of Genesis collectors for specific analyses is also assessed. Thus far, the prevalent model remains viable despite large isotopic variations in a number of volatile elements, but its validity and limitations can be further checked by several Objectives.
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Affiliation(s)
- D. S. Burnett
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCalifornia91125USA
| | - A. J. G. Jurewicz
- Center for Meteorite Studies/School of Earth and Space ExplorationArizona State UniversityTempeArizona85287–1404USA
- Department of Earth SciencesDartmouth CollegeHanoverNew Hampshire03755USA
| | - D. S. Woolum
- Department of PhysicsCalifornia State UniversityFullertonCalifornia92831USA
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Laming JM, Heber VS, Burnett DS, Guan Y, Hervig R, Huss GR, Jurewicz AJG, Koeman-Shields EC, McKeegan KD, Nittler L, Reisenfeld DB, Rieck KD, Wang J, Wiens RC, Woolum DS. DETERMINING THE ELEMENTAL AND ISOTOPIC COMPOSITION OF THE PRESOLAR NEBULA FROM GENESIS DATA ANALYSIS: THE CASE OF OXYGEN. Astrophys J Lett 2017; 851:L12. [PMID: 29657703 PMCID: PMC5893144 DOI: 10.3847/2041-8213/aa9bf0] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
We compare element and isotopic fractionations measured in solar wind samples collected by NASA's Genesis mission with those predicted from models incorporating both the ponderomotive force in the chromosphere and conservation of the first adiabatic invariant in the low corona. Generally good agreement is found, suggesting that these factors are consistent with the process of solar wind fractionation. Based on bulk wind measurements, we also consider in more detail the isotopic and elemental abundances of O. We find mild support for an O abundance in the range 8.75 - 8.83, with a value as low as 8.69 disfavored. A stronger conclusion must await solar wind regime specific measurements from the Genesis samples.
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Affiliation(s)
- J Martin Laming
- Space Science Division, Naval Research Laboratory, Code 7684, Washington DC 20375
| | - V S Heber
- Dept. of Earth, Planetary & Space Sciences UCLA, Los Angeles CA 90095
| | - D S Burnett
- Div. of Geological & Planetary Sciences, Caltech, Pasadena CA 91125
| | - Y Guan
- Div. of Geological & Planetary Sciences, Caltech, Pasadena CA 91125
| | - R Hervig
- School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85287
| | - G R Huss
- Hawaii Institute of Geophysics & Planetology, University of Hawaii at Manoa, 1680 East-West Road, Honolulu, HI 96822
| | - A J G Jurewicz
- School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85287
| | - E C Koeman-Shields
- Hawaii Institute of Geophysics & Planetology, University of Hawaii at Manoa, 1680 East-West Road, Honolulu, HI 96822
| | - K D McKeegan
- Dept. of Earth, Planetary & Space Sciences UCLA, Los Angeles CA 90095
| | - L Nittler
- Department of Terrestrial Magnetism, Carnegie Institute of Washington, Washington DC 20015
| | - D B Reisenfeld
- Department of Physics, University of Montana, Missoula, MT 59812
| | - K D Rieck
- Space and Remote Sensing (ISR-2), LANL, Los Alamos NM 877545
| | - J Wang
- Department of Terrestrial Magnetism, Carnegie Institute of Washington, Washington DC 20015
| | - R C Wiens
- Space and Remote Sensing (ISR-2), LANL, Los Alamos NM 877545
| | - D S Woolum
- Department of Physics, CSUF, Fullerton CA 92831
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Wasserburg GJ, Huneke JC, Burnett DS. Correlation between fission tracks and fission type xenon in meteoritic Whitlockite. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb074i017p04221] [Citation(s) in RCA: 83] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Eugster O, Tera F, Burnett DS, Wasserburg GJ. Isotopic composition of gadolinium and neutron-capture effects in some meteorites. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb075i014p02753] [Citation(s) in RCA: 101] [Impact Index Per Article: 8.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Marty B, Chaussidon M, Wiens RC, Jurewicz AJG, Burnett DS. A 15N-poor isotopic composition for the solar system as shown by Genesis solar wind samples. Science 2011; 332:1533-6. [PMID: 21700869 DOI: 10.1126/science.1204656] [Citation(s) in RCA: 210] [Impact Index Per Article: 16.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Genesis mission sampled solar wind ions to document the elemental and isotopic compositions of the Sun and, by inference, of the protosolar nebula. Nitrogen was a key target element because the extent and origin of its isotopic variations in solar system materials remain unknown. Isotopic analysis of a Genesis Solar Wind Concentrator target material shows that implanted solar wind nitrogen has a (15)N/(14)N ratio of 2.18 ± 0.02 × 10(-3) (that is, ≈40% poorer in (15)N relative to terrestrial atmosphere). The (15)N/(14)N ratio of the protosolar nebula was 2.27 ± 0.03 × 10(-3), which is the lowest (15)N/(14)N ratio known for solar system objects. This result demonstrates the extreme nitrogen isotopic heterogeneity of the nascent solar system and accounts for the (15)N-depleted components observed in solar system reservoirs.
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Affiliation(s)
- B Marty
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Nancy Université, Vandoeuvre-lès-Nancy, France.
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McKeegan KD, Kallio APA, Heber VS, Jarzebinski G, Mao PH, Coath CD, Kunihiro T, Wiens RC, Nordholt JE, Moses RW, Reisenfeld DB, Jurewicz AJG, Burnett DS. The oxygen isotopic composition of the Sun inferred from captured solar wind. Science 2011; 332:1528-32. [PMID: 21700868 DOI: 10.1126/science.1204636] [Citation(s) in RCA: 271] [Impact Index Per Article: 20.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
All planetary materials sampled thus far vary in their relative abundance of the major isotope of oxygen, (16)O, such that it has not been possible to define a primordial solar system composition. We measured the oxygen isotopic composition of solar wind captured and returned to Earth by NASA's Genesis mission. Our results demonstrate that the Sun is highly enriched in (16)O relative to the Earth, Moon, Mars, and bulk meteorites. Because the solar photosphere preserves the average isotopic composition of the solar system for elements heavier than lithium, we conclude that essentially all rocky materials in the inner solar system were enriched in (17)O and (18)O, relative to (16)O, by ~7%, probably via non-mass-dependent chemistry before accretion of the first planetesimals.
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Affiliation(s)
- K D McKeegan
- Department of Earth and Space Sciences, University of California-Los Angeles (UCLA), Los Angeles, CA 90095-1567, USA.
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Veryovkin IV, Tripa CE, Zinovev AV, King BV, Pellin MJ, Burnett DS. RIMS analysis of Ca and Cr in Genesis solar wind collectors. SURF INTERFACE ANAL 2010. [DOI: 10.1002/sia.3523] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Murrell MT, Burnett DS. Partitioning of K, U, and Th between sulfide and silicate liquids: Implications for radioactive heating of planetary cores. ACTA ACUST UNITED AC 1986. [DOI: 10.1029/jb091ib08p08126] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Albee AL, Burnett DS, Chodos AA, Eugster OJ, Huneke JC, Papanastassiou DA, Podosek FA, Russ GP, Sanz HG, Tera F, Wasserburg GJ. Ages, Irradiation History, and Chemical Composition of Lunar Rocks from the Sea of Tranquillity. Science 1970; 167:463-6. [PMID: 17781453 DOI: 10.1126/science.167.3918.463] [Citation(s) in RCA: 87] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The (87)Rb-(87)Sr internal isochrons for five rocks yield an age of 3.65 +/-0.05 x 10(9) years which presumably dates the formation of the Sea of Tranquillity. Potassium-argon ages are consistent with this result. The soil has a model age of 4.5 x10(9) years, which is best regarded as the time of initial differentiation of the lunar crust. A peculiar rock fragment from the soil gave a model age of 4.44 x 10(9) years. Relative abundances of alkalis do not suggest differential volatilization. The irradiation history of lunar rocks is inferred from isotopic measurements of gadolinium, vanadium, and cosmogenic rare gases. Spallation xenon spectra exhibit a high and variable (131)Xe/(126)Xe ratio. No evidence for (129)I was found. The isotopic composition of solar-wind xenon is distinct from that of the atmosphere and of the average for carbonaceous chondrites, but the krypton composition appears similar to average carbonaceous chondrite krypton.
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Plasil F, Burnett DS, Britt HC, Thompson SG. Kinetic Energy—Mass Distributions from the Fission of Nuclei Lighter than Radium. ACTA ACUST UNITED AC 1966. [DOI: 10.1103/physrev.142.696] [Citation(s) in RCA: 85] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
The isotopic compositions and concentrations of rubidium and strontium were determined in silicate nodules contained in Weekeroo Station meteorite, a brecciated coarse octahedrite. The strontium had a Sr(87):Sr(86) range from 0.729 to 0.768, showing considerable enrichment in Sr(87) in coinparison with achondrites. Data for six samples of nodules lie on a straight line on the Sr-Rb evolution diagram, with an initial Sr(87):Sr(86) ratio of 0.696 to 0.702; the slope is 0.0674, corresponding to an age of 4.7 x 10(9) years for lambda = 1.39 x 10(-11) year(-1). These data agree with the previously assigned ages for the formation of stony meteorites and the earth; they support the conclusion that the major period of chemical and physical differentiation in the solar system occurred in a narrow interval at about this time. This result disagrees with the Ar(40)-K(40) ages of 5 to 13 x 10(9) years determined from other iron meteorites. A wide variety of isotopic-age investigations now seem experimentally feasible on iron meteorites that contain silicates.
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