Terrestrial in Situ Cosmogenic Nuclides: Theory and Application John C

Total Page:16

File Type:pdf, Size:1020Kb

Terrestrial in Situ Cosmogenic Nuclides: Theory and Application John C Quaternary Science Reviews 20 (2001) 1475}1560 Terrestrial in situ cosmogenic nuclides: theory and application John C. Gosse *, Fred M. Phillips Department of Geology, 120 Lindley Hall, University of Kansas, Lawrence, KS 66045, USA Department of Earth & Environmental Science, New Mexico Tech, Socorro, NM 87801, USA Abstract The cosmogenic nuclide exposure history method is undergoing major developments in analytical, theoretical, and applied areas. The capability to routinely measure low concentrations of stable and radioactive cosmogenic nuclides has led to new methods for addressing long-standing geologic questions and has provided insights into rates and styles of sur"cial processes. The di!erent physical and chemical properties of the six most widely used nuclides: He, Be, C, Ne, Al, and Cl, make it possible to apply the surface exposure dating methods on rock surfaces of virtually any lithology at any latitude and altitude, for exposures ranging from 10 to 10 years. The terrestrial in situ cosmogenic nuclide method is beginning to revolutionize the manner in which we study landscape evolution. Single or multiple nuclides can be measured in a single rock surface to obtain erosion rates on boulder and bedrock surfaces, #uvial incision rates, denudation rates of individual landforms or entire drainage basins, burial histories of rock surfaces and sediment, scarp retreat, fault slip rates, paleoseismology, and paleoaltimetry. Ages of climatic variations recorded by moraine and alluvium sediments are being directly determined. Advances in our understanding of how cosmic radiation interacts with the geomagnetic "eld and atmosphere will improve numerical simulations of cosmic-ray interactions over any exposure duration and complement additional empirical measurements of nuclide production rates. The total uncertainty in the exposure ages is continually improving. This article presents the theory necessary for interpreting cosmogenic nuclide data, reviews estimates of parameters, describes strategies and practical considerations in "eld applications, and assesses sources of error in interpreting cosmogenic nuclide measurements. 2001 Elsevier Science Ltd. All rights reserved. TABLE OF CONTENTS 1. Introduction ............................................................................................ 1477 1.1. Development of the TCN methods . 1477 1.2. Applications of TCN Exposure methods . 1479 1.3. Previous reviews . 1480 2. Glossary ............................................................................................... 1480 2.1. Terminology . 1480 2.2. Notation . 1482 3. Principles .............................................................................................. 1485 3.1. Introduction . 1485 3.1.1. Source of the primary radiation .............................................................. 1485 3.1.2. Ewects of the geomagnetic xeld on GCR .................................................... 1485 3.1.3. Trajectory models and models of secondary nuclide production rates . 1487 3.1.4. Recent numerical models of GCR particle production ....................................... 1489 3.1.5. Nuclide production from primary GCR ...................................................... 1490 3.1.6. TCN production by energetic nucleons ...................................................... 1491 * Corresponding author. Tel.: #1-785-864-4974; fax: #1-785-864-5276. E-mail address: [email protected] (J.C. Gosse). 0277-3791/01/$ - see front matter 2001 Elsevier Science Ltd. All rights reserved. PII: S 0 2 7 7 - 3 7 9 1 ( 0 0 ) 0 0 1 7 1 - 2 1476 J.C. Gosse, F.M. Phillips / Quaternary Science Reviews 20 (2001) 1475}1560 3.1.7. TCN production by low-energy neutron ...................................................... 1491 3.1.8. TCN production by muons ................................................................... 1492 3.1.9. Factors limiting TCN applications ........................................................... 1493 3.2. Numerical simulation of low-energy neutron behavior . 1493 3.3. Analytical equations for TCN production . 1495 3.3.1. Fast neutron (Spallation) production ........................................................ 1496 3.3.2. Production by epithermal neutrons .......................................................... 1497 3.3.3. Production by thermal neutrons .............................................................. 1498 3.3.4. Production by muons and muon-derived neutrons ........................................... 1499 3.3.5. Total nuclide production ..................................................................... 1502 3.4. Energetic neutron attenuation length. 1502 3.5. Temporal variations in production rates . 1504 3.5.1. Variations in the primary GCR yux .......................................................... 1506 3.5.2. Variations due to solar modulation of the magnetic xeld . 1507 3.5.3. Ewects of the geomagnetic xeld .............................................................. 1507 3.5.4. Variations in atmospheric shielding .......................................................... 1515 3.5.5. Other sources of temporal variations in production ......................................... 1515 3.6. Estimation of production rates . 1516 3.6.1. Helium-3 ...................................................................................... 1516 3.6.2. Beryllium-10 .................................................................................. 1516 3.6.3. Carbon-14 .................................................................................... 1517 3.6.4. Neon-21 ....................................................................................... 1517 3.6.5. Aluminum-26 ................................................................................. 1517 3.6.6. Chlorine-36 ................................................................................... 1518 3.7. Scaling and correction factors for production rates . 1518 3.7.1. Spatial scaling ................................................................................ 1518 3.7.2. Topographic shielding ........................................................................ 1520 3.7.3. Surface coverage ............................................................................. 1522 3.7.4. Sample thickness .............................................................................. 1522 3.7.5. Thermal neutron leakage ..................................................................... 1523 3.8. Exposure dating witha single TCN . 1523 3.9. Exposure dating withmultiple nuclides . 1527 3.10. Nuclide-speci"c considerations . 1531 3.10.1. Helium-3 .................................................................................... 1531 3.10.2. Beryllium-10 ................................................................................. 1531 3.10.3. Carbon-14 ................................................................................... 1532 3.10.4. Neon-21 ..................................................................................... 1532 3.10.5. Aluminum-26 ................................................................................ 1532 3.10.6. Chlorine-36 .................................................................................. 1533 3.11. TCN dating of sediment . 1533 4. Sampling strategies .................................................................................... 1536 4.1. Field sampling considerations . 1536 4.1.1. Sample description ........................................................................... 1536 4.1.2. Sampling methodology ....................................................................... 1537 4.2. Other lithological considerations . 1538 4.3. How muchsample is needed? . 1538 4.4. Strategies for concentration-depthpro "les . 1539 5. Sample preparation and experimental data interpretation ........................................... 1540 5.1. TCN sample preparation . 1540 5.1.1. Preparation time .............................................................................. 1541 5.1.2. Physical and chemical pretreatment ......................................................... 1541 5.1.3. Isotopic extraction ............................................................................ 1541 5.2. Experimental data interpretation . 1542 6. Uncertainty and sources of error ..................................................................... 1544 6.1. Sources of error . 1544 6.1.1. Sample characteristics ........................................................................ 1545 6.1.2. Sample preparation and elemental analyses ................................................. 1546 J.C. Gosse, F.M. Phillips / Quaternary Science Reviews 20 (2001) 1475}1560 1477 6.1.3. Mass spectrometry ............................................................................ 1546 6.1.4. Systematic errors ............................................................................. 1547 6.2. Reporting the uncertainty . 1548 6.2.1. Error propagation ............................................................................ 1549 6.2.2. Evaluating accuracy by intercomparison .................................................... 1549 6.2.3. Multiple sample measurements ............................................................... 1550 6.2.4. Sensitivity analysis ........................................................................... 1550 7. Directions of future contributions .................................................................... 1550 Acknowledgements ...................................................................................
Recommended publications
  • Subterranean Production of Neutrons, $^{39} $ Ar and $^{21} $ Ne: Rates
    Subterranean production of neutrons, 39Ar and 21Ne: Rates and uncertainties Ondrejˇ Srˇ amek´ a,∗, Lauren Stevensb, William F. McDonoughb,c,∗∗, Sujoy Mukhopadhyayd, R. J. Petersone aDepartment of Geophysics, Faculty of Mathematics and Physics, Charles University, V Holeˇsoviˇck´ach 2, 18000 Praha 8, Czech Republic bDepartment of Chemistry and Biochemistry, University of Maryland, College Park, MD 20742, United States cDepartment of Geology, University of Maryland, College Park, MD 20742, United States dDepartment of Earth and Planetary Sciences, University of California Davis, Davis, CA 95616, United States eDepartment of Physics, University of Colorado Boulder, Boulder, CO 80309-0390, United States Abstract Accurate understanding of the subsurface production rate of the radionuclide 39Ar is necessary for argon dating tech- niques and noble gas geochemistry of the shallow and the deep Earth, and is also of interest to the WIMP dark matter experimental particle physics community. Our new calculations of subsurface production of neutrons, 21Ne, and 39Ar take advantage of the state-of-the-art reliable tools of nuclear physics to obtain reaction cross sections and spectra (TALYS) and to evaluate neutron propagation in rock (MCNP6). We discuss our method and results in relation to pre- vious studies and show the relative importance of various neutron, 21Ne, and 39Ar nucleogenic production channels. Uncertainty in nuclear reaction cross sections, which is the major contributor to overall calculation uncertainty, is estimated from variability in existing experimental and library data. Depending on selected rock composition, on the order of 107–1010 α particles are produced in one kilogram of rock per year (order of 1–103 kg−1 s−1); the number of produced neutrons is lower by ∼ 6 orders of magnitude, 21Ne production rate drops by an additional factor of 15–20, and another one order of magnitude or more is dropped in production of 39Ar.
    [Show full text]
  • Monitored Natural Attenuation of Inorganic Contaminants in Ground
    Monitored Natural Attenuation of Inorganic Contaminants in Ground Water Volume 3 Assessment for Radionuclides Including Tritium, Radon, Strontium, Technetium, Uranium, Iodine, Radium, Thorium, Cesium, and Plutonium-Americium EPA/600/R-10/093 September 2010 Monitored Natural Attenuation of Inorganic Contaminants in Ground Water Volume 3 Assessment for Radionuclides Including Tritium, Radon, Strontium, Technetium, Uranium, Iodine, Radium, Thorium, Cesium, and Plutonium-Americium Edited by Robert G. Ford Land Remediation and Pollution Control Division Cincinnati, Ohio 45268 and Richard T. Wilkin Ground Water and Ecosystems Restoration Division Ada, Oklahoma 74820 Project Officer Robert G. Ford Land Remediation and Pollution Control Division Cincinnati, Ohio 45268 National Risk Management Research Laboratory Office of Research and Development U.S. Environmental Protection Agency Cincinnati, Ohio 45268 Notice The U.S. Environmental Protection Agency through its Office of Research and Development managed portions of the technical work described here under EPA Contract No. 68-C-02-092 to Dynamac Corporation, Ada, Oklahoma (David Burden, Project Officer) through funds provided by the U.S. Environmental Protection Agency’s Office of Air and Radiation and Office of Solid Waste and Emergency Response. It has been subjected to the Agency’s peer and administrative review and has been approved for publication as an EPA document. Mention of trade names or commercial products does not constitute endorsement or recommendation for use. All research projects making conclusions or recommendations based on environmental data and funded by the U.S. Environmental Protection Agency are required to participate in the Agency Quality Assurance Program. This project did not involve the collection or use of environmental data and, as such, did not require a Quality Assurance Plan.
    [Show full text]
  • Tracer Applications of Noble Gas Radionuclides in the Geosciences
    To be published in Earth-Science Reviews Tracer Applications of Noble Gas Radionuclides in the Geosciences (August 20, 2013) Z.-T. Lua,b, P. Schlosserc,d, W.M. Smethie Jr.c, N.C. Sturchioe, T.P. Fischerf, B.M. Kennedyg, R. Purtscherth, J.P. Severinghausi, D.K. Solomonj, T. Tanhuak, R. Yokochie,l a Physics Division, Argonne National Laboratory, Argonne, Illinois, USA b Department of Physics and Enrico Fermi Institute, University of Chicago, Chicago, USA c Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York, USA d Department of Earth and Environmental Sciences and Department of Earth and Environmental Engineering, Columbia University, New York, USA e Department of Earth and Environmental Sciences, University of Illinois at Chicago, Chicago, IL, USA f Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, USA g Center for Isotope Geochemistry, Lawrence Berkeley National Laboratory, Berkeley, USA h Climate and Environmental Physics, Physics Institute, University of Bern, Bern, Switzerland i Scripps Institution of Oceanography, University of California, San Diego, USA j Department of Geology and Geophysics, University of Utah, Salt Lake City, USA k GEOMAR Helmholtz Center for Ocean Research Kiel, Marine Biogeochemistry, Kiel, Germany l Department of Geophysical Sciences, University of Chicago, Chicago, USA Abstract 81 85 39 Noble gas radionuclides, including Kr (t1/2 = 229,000 yr), Kr (t1/2 = 10.8 yr), and Ar (t1/2 = 269 yr), possess nearly ideal chemical and physical properties for studies of earth and environmental processes. Recent advances in Atom Trap Trace Analysis (ATTA), a laser-based atom counting method, have enabled routine measurements of the radiokrypton isotopes, as well as the demonstration of the ability to measure 39Ar in environmental samples.
    [Show full text]
  • EXTRACTION of BERYLLIUM-10 from SOIL by FUSION Summary
    EXTRACTION OF BERYLLIUM-10 FROM SOIL BY FUSION Summary This method is used to separate Be from soil and sediment samples, for AMS analysis. After adding Be carrier, the sample is fused with KHF2. Be is extracted from the fusion cake with hot water. K is removed by precipitation, the sample is dried to expel fluoride, and Be is recovered as Be(OH)2. Yields are typically 70-80 %, but can be increased by additional leaching of the fusion cake. Version Written by John Stone, 1996-2002. This version revised May 2004 by Greg Balco. Available at: http://depts.washington.edu/cosmolab/chem.html References If you use this method, please cite: Stone, J.O.H. (1998). A rapid fusion method for the extraction of Be-10 from soils and silicates. Geochimica et Cosmochimica Acta (Scientific comment) 62, 555-561. Sampling and grinding Mix and grind an unbiased ∼ 50-100 g sample of the material. If possible, mix the original sample bag before opening and take representative proportions of coarse and fine material. Fine soil, carbonate nodules, clay lumps, rock fragments, etc., all have different 10Be concentrations. Grinding homogenises the sample and ensures that these components are evenly represented in the small subsample used for the analysis. If the sample is wet, you will need to dry it before grinding. Initial sample drying Samples are best run in batches of four. This is because we currently have four Pt crucibles. Given more crucibles and sufficient hotplate space, batches of 8 or even 12 are equally feasible. ————————————————— UW Cosmogenic Nuclide Lab – 10Be fusion process 1 – Label and tare four disposable aluminum foil drying dishes and transfer a few grams of ground sediment to each with a steel spatula.
    [Show full text]
  • Isotopegeochemistry Chapter4
    Isotope Geochemistry W. M. White Chapter 4 GEOCHRONOLOGY III: OTHER DATING METHODS 4.1 COSMOGENIC NUCLIDES 4.1.1 Cosmic Rays in the Atmosphere As the name implies, cosmogenic nuclides are produced by cosmic rays colliding with atoms in the atmosphere and the surface of the solid Earth. Nuclides so created may be stable or radioactive. Radio- active cosmogenic nuclides, like the U decay series nuclides, have half-lives sufficiently short that they would not exist in the Earth if they were not continually produced. Assuming that the production rate is constant through time, then the abundance of a cosmogenic nuclide in a reservoir isolated from cos- mic ray production is simply given by: −λt N = N0e 4.1 Hence if we know N0 and measure N, we can calculate t. Table 4.1 lists the radioactive cosmogenic nu- clides of principal interest. As we shall, cosmic ray interactions can also produce rare stable nuclides, and their abundance can also be used to measure geologic time. A number of different nuclear reactions create cosmogenic nuclides. “Cosmic rays” are high-energy (several GeV up to 1019 eV!) atomic nuclei, mainly of H and He (because these constitute most of the matter in the universe), but nuclei of all the elements have been recognized. To put these kinds of ener- gies in perspective, the previous gen- eration of accelerators for physics ex- Table 4.1. Data on Cosmogenic Nuclides periments, such as the Cornell Elec- -1 tron Storage Ring produce energies in Nuclide Half-life, years Decay constant, yr the 10’s of GeV (1010 eV); while 14C 5730 1.209x 10-4 CERN’s Large Hadron Collider, 3H 12.33 5.62 x 10-2 mankind’s most powerful accelerator, 10Be 1.500 × 106 4.62 x 10-7 located on the Franco-Swiss border 26Al 7.16 × 105 9.68x 10-5 near Geneva produces energies of 36Cl 3.08 × 105 2.25x 10-6 ~10 TeV range (1013 eV).
    [Show full text]
  • Radiogenic Isotope Geochemistry
    W. M. White Geochemistry Chapter 8: Radiogenic Isotope Geochemistry CHAPTER 8: RADIOGENIC ISOTOPE GEOCHEMISTRY 8.1 INTRODUCTION adiogenic isotope geochemistry had an enormous influence on geologic thinking in the twentieth century. The story begins, however, in the late nineteenth century. At that time Lord Kelvin (born William Thomson, and who profoundly influenced the development of physics and ther- R th modynamics in the 19 century), estimated the age of the solar system to be about 100 million years, based on the assumption that the Sun’s energy was derived from gravitational collapse. In 1897 he re- vised this estimate downward to the range of 20 to 40 million years. A year earlier, another Eng- lishman, John Jolly, estimated the age of the Earth to be about 100 million years based on the assump- tion that salts in the ocean had built up through geologic time at a rate proportional their delivery by rivers. Geologists were particularly skeptical of Kelvin’s revised estimate, feeling the Earth must be older than this, but had no quantitative means of supporting their arguments. They did not realize it, but the key to the ultimate solution of the dilemma, radioactivity, had been discovered about the same time (1896) by Frenchman Henri Becquerel. Only eleven years elapsed before Bertram Boltwood, an American chemist, published the first ‘radiometric age’. He determined the lead concentrations in three samples of pitchblende, a uranium ore, and concluded they ranged in age from 410 to 535 million years. In the meantime, Jolly also had been busy exploring the uses of radioactivity in geology and published what we might call the first book on isotope geochemistry in 1908.
    [Show full text]
  • Meteoric Be and Be As Process Tracers in the Environment
    Chapter 5 Meteoric 7Be and 10Be as Process Tracers in the Environment James M. Kaste and Mark Baskaran 7 10 Abstract Be (T1/2 ¼ 53 days) and Be (T1/2 ¼ occurring Be isotopes of use to Earth scientists are the 7 1.4 Ma) form via natural cosmogenic reactions in the short-lived Be (T1/2 ¼ 53.1 days) and the longer- 10 atmosphere and are delivered to Earth’s surface by wet lived Be (T1/2 ¼ 1.4 Ma; Nishiizumi et al. 2007). and dry deposition. The distinct source term and near- Because cosmic rays that cause the initial cascade of constant fallout of these radionuclides onto soils, vege- neutrons and protons in the upper atmosphere respon- tation, waters, ice, and sediments makes them valuable sible for the spallation reactions are attenuated by tracers of a wide range of environmental processes the mass of the atmosphere itself, production rates of operating over timescales from weeks to millions of comsogenic Be are three orders of magnitude higher in years. Beryllium tends to form strong bonds with oxygen the stratosphere than they are at sea-level (Masarik and atoms, so 7Be and 10Be adsorb rapidly to organic and Beer 1999, 2009). Most of the production of cosmo- inorganic solid phases in the terrestrial and marine envi- genic Be therefore occurs in the upper atmosphere ronment. Thus, cosmogenic isotopes of beryllium can be (5–30 km), although there is trace, but measurable used to quantify surface age, sediment source, mixing production as oxygen atoms in minerals at the Earth’s rates, and particle residence and transit times in soils, surface are spallated (in situ produced; see Lal 2011, streams, lakes, and the oceans.
    [Show full text]
  • Nucleosynthesis
    Nucleosynthesis Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. Seventeen minutes later the universe had cooled to a point at which these processes ended, so only the fastest and simplest reactions occurred, leaving our universe containing about 75% hydrogen, 24% helium, and traces of other elements such aslithium and the hydrogen isotope deuterium. The universe still has approximately the same composition today. Heavier nuclei were created from these, by several processes. Stars formed, and began to fuse light elements to heavier ones in their cores, giving off energy in the process, known as stellar nucleosynthesis. Fusion processes create many of the lighter elements up to and including iron and nickel, and these elements are ejected into space (the interstellar medium) when smaller stars shed their outer envelopes and become smaller stars known as white dwarfs. The remains of their ejected mass form theplanetary nebulae observable throughout our galaxy. Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28).[1] Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic process) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the r-process) in the period of a few seconds during the explosion.
    [Show full text]
  • Beryllium-10 Terrestrial Cosmogenic Nuclide Surface Exposure Dating of Quaternary Landforms in Death Valley
    Geomorphology 125 (2011) 541–557 Contents lists available at ScienceDirect Geomorphology journal homepage: www.elsevier.com/locate/geomorph Beryllium-10 terrestrial cosmogenic nuclide surface exposure dating of Quaternary landforms in Death Valley Lewis A. Owen a,⁎, Kurt L. Frankel b, Jeffrey R. Knott c, Scott Reynhout a, Robert C. Finkel d,e, James F. Dolan f, Jeffrey Lee g a Department of Geology, University of Cincinnati, Cincinnati, Ohio, USA b School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA 30332, USA c Department of Geological Sciences, California State University, Fullerton, California, USA d Department of Earth and Planetary Science Department, University of California, Berkeley, Berkeley, CA 94720-4767, USA e CEREGE, BP 80 Europole Méditerranéen de l'Arbois, 13545 Aix en Provence Cedex 4, France f Department of Earth Sciences, University of Southern California, Los Angeles, California, USA g Department of Geological Sciences, Central Washington University, Ellensburg, Washington, USA article info abstract Article history: Quaternary alluvial fans, and shorelines, spits and beach bars were dated using 10Be terrestrial cosmogenic Received 10 March 2010 nuclide (TCN) surface exposure methods in Death Valley. The 10Be TCN ages show considerable variance on Received in revised form 3 October 2010 individual surfaces. Samples collected in the active channels date from ~6 ka to ~93 ka, showing that there is Accepted 18 October 2010 significant 10Be TCN inheritance within cobbles and boulders. This
    [Show full text]
  • Lecture 12: Cosmogenic Isotopes In
    Geol. 655 Isotope Geochemistry Lecture 12 Spring 2007 GEOCHRONOLOGY VIII: COSMOGENIC NUCLIDES INTRODUCTION As the name implies, cosmogenic nuclides are produced by cosmic rays, specifically by collisions with atoms in the atmosphere (and to a much lesser extent, the surface of the solid Earth). Nuclides so created may be stable or radioactive. Radioactive cosmogenic nuclides, like the U decay series nuclides, have half-lives sufficiently short that they would not exist in the Earth if they were not continually pro- duced. Assuming that the production rate is constant through time, then the abundance of a cos- mogenic nuclide in a reservoir isolated from cosmic ray production is simply given by: !"t N = N0e 12.1 Hence if we know N0 and measure N, we can calculate t. Table 12.1 lists the radioactive cosmogenic nuclides of principal interest. As we shall see in the next lecture, cosmic ray interactions can also produce TABLE 12.1. COSMOGENIC NUCLIDES OF GEOLOGICAL INTEREST rare stable nuclides, and their abun- Nuclide Half-life, years Decay constant, y-1 dance can also be used to measure 14C 5730 1.209x 10-3 geologic time. 3H 12.33 5.62 x 10-2 Cosmogenic nuclides are created 10Be 1.500 × 106 4.62 x 10-5 by a number of nuclear reactions 26Al 7.16 × 105 9.68x 10-5 with cosmic rays and by-products of 36Cl 3.08 × 105 2.25x 10-6 cosmic rays. “Cosmic rays” are high 32Si 276 2.51x 10-2 energy (several GeV up to 1019 eV!!) charged particles, mainly protons, or H nuclei (since, after all, H constitutes most of the matter in the universe), but nuclei of all the elements have been recognized.
    [Show full text]
  • Polar Desert Chronologies Through Quantitative Measurements of Salt Accumulation
    Polar desert chronologies through quantitative measurements of salt accumulation Joseph A. Graly1, Kathy J. Licht1, Gregory K. Druschel1, and Michael R. Kaplan2 1Department of Earth Sciences, Indiana University–Purdue University Indianapolis, Indianapolis, Indiana 46202, USA 2Lamont–Doherty Earth Observatory, Palisades, New York 10964, USA ABSTRACT isotopes suggest a primarily atmospheric ori- We measured salt concentration and speciation in the top horizons of moraine sediments gin, with some trace mineral boron (Leslie et from the Transantarctic Mountains (Antarctica) and compared the salt data to cosmogenic- al., 2014). However, the Dry Valleys boron iso- nuclide exposure ages on the same moraine. Because the salts are primarily of atmospheric tope values that suggest a trace mineral compo- origin, and their delivery to the sediment is constant over relevant time scales, a linear rate of nent could also form from Rayleigh distillation accumulation is expected. When salts are measured in a consistent grain-size fraction and at during the precipitation of atmospheric boron a consistent position within the soil column, a linear correlation between salt concentration (Rose-Koga et al., 2006). and exposure age is evident. This correlation is strongest for boron-containing salts (R2 > 0.99), Atmospheric aerosols exist either as acid 2 but is also strong (R ≈ 0.9) for most other water-extracted salt species. The relative mobility vapors and gases (e.g., HNO3, N2O5, etc.) or of salts in the soil column does not correspond to species solubility (borate is highly soluble). as anion-cation pairs, commonly adhering to Instead, the highly consistent behavior of boron within the soil column is best explained by particulate matter.
    [Show full text]
  • Cosmogenic and Nucleogenic 21Ne in Quartz in a 28-Meter Sandstone Core from the Mcmurdo Dry Valleys, Antarctica
    Cosmogenic and nucleogenic 21Ne in quartz in a 28-meter sandstone core from the McMurdo Dry Valleys, Antarctica Greg Balco∗,a, Pierre-Henri Blardb, David L. Shusterd,a, John O.H. Stonec, Laurent Zimmermannb a Berkeley Geochronology Center, 2455 Ridge Road, Berkeley CA 94709 USA b CRPG, CNRS-Universit´ede Lorraine, UMR 7358, 15 rue Notre Dame des Pauvres, 54501 Vandoeuvre-l`es-Nancy, France c Earth and Space Sciences, University of Washington, Seattle WA USA d Department of Earth and Planetary Science, 479 McCone Hall, University of California, Berkeley CA 94720, USA Abstract We measured concentrations of Ne isotopes in quartz in a 27.6-meter sandstone core from a low-erosion-rate site at 2183 m elevation at Beacon Heights in the Antarc- tic Dry Valleys. Surface concentrations of cosmogenic 21Ne indicate a surface exposure age of at least 4.1 Ma and an erosion rate no higher than ca. 14 cm Myr−1. 21Ne con- centrations in the upper few centimeters of the core show evidence for secondary spal- logenic neutron escape effects at the rock surface, which is predicted by first-principles models of cosmogenic-nuclide production but is not commonly observed in natural examples. We used a model for 21Ne production by various mechanisms fit to the ob- servations to distinguish cosmic-ray-produced 21Ne from nucleogenic 21Ne produced by decay of trace U and Th present in quartz, and also constrain rates of subsurface 21Ne production by cosmic-ray muons. Core samples have a quartz (U-Th)/Ne closure age, reflecting cooling below approximately 95°C, near 160 Ma, which is consistent with existing apatite fission-track data and the 183 Ma emplacement of nearby Ferrar dolerite intrusions.
    [Show full text]