Soil, Regolith, and Weathered Rock Theoretical Concepts and Evolution
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The Effect of Time on Soil Development: Study of a Soil Chronosequence from Reunion Island, Indian Ocean
University of Wollongong Research Online Faculty of Science, Medicine & Health - Honours Theses University of Wollongong Thesis Collections 2016 The effect of time on soil development: study of a soil chronosequence from Reunion Island, Indian Ocean Alex Hannan-Joyner Follow this and additional works at: https://ro.uow.edu.au/thsci University of Wollongong Copyright Warning You may print or download ONE copy of this document for the purpose of your own research or study. The University does not authorise you to copy, communicate or otherwise make available electronically to any other person any copyright material contained on this site. You are reminded of the following: This work is copyright. Apart from any use permitted under the Copyright Act 1968, no part of this work may be reproduced by any process, nor may any other exclusive right be exercised, without the permission of the author. Copyright owners are entitled to take legal action against persons who infringe their copyright. A reproduction of material that is protected by copyright may be a copyright infringement. A court may impose penalties and award damages in relation to offences and infringements relating to copyright material. Higher penalties may apply, and higher damages may be awarded, for offences and infringements involving the conversion of material into digital or electronic form. Unless otherwise indicated, the views expressed in this thesis are those of the author and do not necessarily represent the views of the University of Wollongong. Recommended Citation Hannan-Joyner, Alex, The effect of time on soil development: study of a soil chronosequence from Reunion Island, Indian Ocean, BSci Hons, School of Earth & Environmental Sciences, University of Wollongong, 2016. -
Biomechanical and Biochemical Effects Recorded in the Tree Root Zone – Soil Memory, Historical Contingency and Soil Evolution Under Trees
Plant Soil (2018) 426:109–134 https://doi.org/10.1007/s11104-018-3622-9 REGULAR ARTICLE Biomechanical and biochemical effects recorded in the tree root zone – soil memory, historical contingency and soil evolution under trees Łukasz Pawlik & Pavel Šamonil Received: 17 September 2017 /Accepted: 1 March 2018 /Published online: 15 March 2018 # The Author(s) 2018 Abstract increase in soil spatial complexity. We hypothesized that Background and aims The changing soils is a never- trees can be a strong local factor intensifying, blocking ending process moderated by numerous biotic and abi- or modifying pedogenetic processes, leading to local otic factors. Among these factors, trees may play a changes in soil complexity (convergence, divergence, critical role in forested landscapes by having a large or polygenesis). These changes are hypothetically con- imprint on soil texture and chemical properties. During trolled by regionally predominating soil formation their evolution, soils can follow convergent or divergent processes. development pathways, leading to a decrease or an Methods To test the main hypothesis, we described the pedomorphological features of soils under tree stumps of fir, beech and hemlock in three soil regions: Haplic Highlights Cambisols (Turbacz Reserve, Poland), Entic Podzols 1) The architecture of tree root systems controls soil physical and (Žofínský Prales Reserve, Czech Republic) and Albic chemical properties. Podzols (Upper Peninsula, Michigan, USA). Soil pro- 2) The predominating pedogenetic process significantly modifies files under the stumps, as well as control profiles on sites the effect of trees on soil. 3) Trees are a factor in polygenesis in Haplic Cambisols at the currently not occupied by trees, were analyzed in the pedon scale. -
Deficit Saline Water Irrigation Under Reduced Tillage and Residue Mulch
www.nature.com/scientificreports OPEN Defcit saline water irrigation under reduced tillage and residue mulch improves soil health in sorghum‑wheat cropping system in semi‑arid region Pooja Gupta Soni1,2, Nirmalendu Basak 1*, Arvind Kumar Rai 1*, Parul Sundha1, Bhaskar Narjary1, Parveen Kumar1, Gajender Yadav1, Satyendra Kumar1 & Rajender Kumar Yadav1 Judicious application of saline water except for critical growth stages, could be the only practical solution to meet the crop water demand in arid and semi‑arid regions, due to limited access to freshwater, especially during dry winter months. A feld experiment was conducted to study the efect of tillage [conventional (CT), reduced (RT), and zero (ZT)], rice straw mulch and defcit saline‑water irrigation in wheat (100, 80 and 60% of wheat water requirement, CWR) followed by rainfed sorghum on soil properties and the yields of the cropping system. Yields of both the crops were comparable between RT and CT, but the wheat yield was reduced in ZT. The RT, mulching and defcit saline irrigation in wheat season (60% CWR) increased the sorghum fodder yield. Olsen’s P (8.7–20.6%) and NH4OAc‑K (2.5–7.5%) increased in RT and ZT, respectively, over CT under both the crops. Defcit −1 irrigation reduced soil salinity (ECe) by 0.73–1.19 dS m after each crop cycle, while soil microbial biomass C (MBC) and N (MBN), dehydrogenase, urease and alkaline phosphatase reduced with an increase in ECe. The α‑glucosidase, MBC, ECe, KMnO4oxidizable N, and urease were identifed as major contributors in developing the soil health index. -
16. Ice in the Martian Regolith
16. ICE IN THE MARTIAN REGOLITH S. W. SQUYRES Cornell University S. M. CLIFFORD Lunar and Planetary Institute R. O. KUZMIN V.I. Vernadsky Institute J. R. ZIMBELMAN Smithsonian Institution and F. M. COSTARD Laboratoire de Geographie Physique Geologic evidence indicates that the Martian surface has been substantially modified by the action of liquid water, and that much of that water still resides beneath the surface as ground ice. The pore volume of the Martian regolith is substantial, and a large amount of this volume can be expected to be at tem- peratures cold enough for ice to be present. Calculations of the thermodynamic stability of ground ice on Mars suggest that it can exist very close to the surface at high latitudes, but can persist only at substantial depths near the equator. Impact craters with distinctive lobale ejecta deposits are common on Mars. These rampart craters apparently owe their morphology to fluidhation of sub- surface materials, perhaps by the melting of ground ice, during impact events. If this interpretation is correct, then the size frequency distribution of rampart 523 524 S. W. SQUYRES ET AL. craters is broadly consistent with the depth distribution of ice inferred from stability calculations. A variety of observed Martian landforms can be attrib- uted to creep of the Martian regolith abetted by deformation of ground ice. Global mapping of creep features also supports the idea that ice is present in near-surface materials at latitudes higher than ± 30°, and suggests that ice is largely absent from such materials at lower latitudes. Other morphologic fea- tures on Mars that may result from the present or former existence of ground ice include chaotic terrain, thermokarst and patterned ground. -
Towards a Prediction of Landscape Evolution from Chemical Weathering and Soil Production
TOWARDS A PREDICTION OF LANDSCAPE EVOLUTION FROM CHEMICAL WEATHERING AND SOIL PRODUCTION A thesis submitted in partial fulfillment of the requirements for the degree of Master of Science By ERIC ALAN JACKSON B.S., Wright State University, 2013 2017 Wright State University WRIGHT STATE UNIVERSITY GRADUATE SCHOOL December 15, 2017 I HEREBY RECOMMEND THAT THE THESIS PREPARED UNDER MY SUPERVISION BY Eric Alan Jackson ENTITLED Towards a Prediction of Landscape Evolution from Chemical Weathering and Soil Production BE ACCEPTED IN PARTIAL FULFLLMENT OF THE REQUIREMENTS FOR THE DEGREE OF Master of Science. __________________________ Allen Hunt, Ph.D. Thesis Director __________________________ Jason Deibel, Ph.D. Chair, Department of Physics Committee on Final Examination _________________________ Thomas Skinner, Ph.D. _________________________ Jerry Clark, Ph.D. _________________________ Barry Milligan, Ph.D. Interim Dean of the Graduate School ABSTRACT Jackson, Eric Alan. M.S. Department of Physics, Wright State University, 2017. Towards a Prediction of Landscape Evolution from Chemical Weathering and Soil Production. The time evolution of a periodic landscape under the influence of chemical weathering and physical erosion is computed. The model used incorporates weathering and soil production as a flux limited reaction controlled by groundwater flow. Scaling of the flow rate is obtained from a percolation theoretic treatment. The erosion of the soil material produced by this process is modeled by the diffusion of elevation, as consistent with downslope soil transport proportional to the tangent of the angle of the topography, and application of the equation of continuity to surface soil transport. Three initial topographies are examined over a periods of thousands of years and resulting landforms and soil productivity compared. -
Surface Residence Times of Regolith on the Lunar Maria
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1652.pdf 1 1 SURFACE RESIDENCE TIMES OF REGOLITH ON THE LUNAR MARIA. P. O’Brien and S. Byrne , 1 L unar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721 ([email protected]) Introduction: The surfaces of airless bodies like Our model simulates mare-like surfaces evolving the Moon undergo microscopic chemical changes as a over time from flat surfaces to cratered landscapes. result of energetic processes operating in the space Impacts are randomly sampled from the present-day environment, collectively known as space weathering lunar impact flux [5] and the global population of [1,2]. Despite returned lunar soil samples, the rate of secondary craters produced by these impacts is space weathering on the Moon is not well understood. generated following empirical observations of The amount of chemical weathering incurred in the secondary production on airless bodies [6,7]. At each lunar regolith depends critically on the rate at which timestep, we compute the downslope flux of regolith regolith is excavated, transported, and buried by by solving the 2D diffusion equation [8]. The rate of macroscopic impact processes. These physical diffusion is calibrated by matching the average processes control how long regolith spends on the roughness of the model landscapes to the observed surface where it is exposed to the space environment. roughness of the lunar maria, as measured by the We have developed a Monte Carlo model that median bidirectional slope at 4 m baselines [9]. Figure simulates the evolution of lunar maria landscapes 1 shows how model surfaces subject to these physical under topographic relief-creation from impact cratering processes become rougher and more heavily-cratered and relief-reduction from micrometeorite gardening over time. -
NASA Spacecraft Nears Encounter with Dwarf Planet Ceres 4 March 2015
NASA spacecraft nears encounter with dwarf planet Ceres 4 March 2015 of 590 miles (950 kilometers), makes a full rotation every nine hours, and NASA is hoping for a wealth of data once the spacecraft's orbit begins. "Dawn is about to make history," said Robert Mase, project manager for the Dawn mission at NASA JPL in Pasadena, California. "Our team is ready and eager to find out what Ceres has in store for us." Experts will be looking for signs of geologic activity, via changes in these bright spots, or other features on Ceres' surface over time. The latest images came from Dawn when it was 25,000 miles (40,000 kilometers) away on February 25. This image was taken by NASA's Dawn spacecraft of dwarf planet Ceres on February 19, 2015 from a The celestial body was first spotted by Sicilian distance of nearly 29,000 miles astronomer Father Giuseppe Piazzi in 1801. "Ceres was initially classified as a planet and later called an asteroid. In recognition of its planet-like A NASA spacecraft called Dawn is about to qualities, Ceres was designated a dwarf planet in become the first mission to orbit a dwarf planet 2006, along with Pluto and Eris," NASA said. when it slips into orbit Friday around Ceres, the most massive body in the asteroid belt. Ceres is named after the Roman goddess of agriculture and harvests. The mission aims to shed light on the origins of the solar system 4.5 billion years ago, from its "rough The spacecraft on its way to circle it was launched and tumble environment of the main asteroid belt in September 2007. -
Global Rates of Soil Production Independent of Soil Depth 2 Authors: Emma J
Non-peer reviewed preprint submitted to EarthArXiv 1 Global rates of soil production independent of soil depth 2 Authors: Emma J. Harrison1,2*, Jane K. Willenbring1,2, Gilles Y. Brocard3 3 Affiliations: 4 1 Scripps Institution of Oceanography, University of California San Diego, La Jolla, CA, USA 5 2 Now at Geological Sciences, Stanford University, Stanford, CA, USA 6 3Archéorient, UMR 5133, Maison de l’Orient et de la Mediterranée, University of Lyon 2, 7 France. 8 *corresponding author email : [email protected] 9 ABSTRACT 10 Accelerated rates of soil erosion threaten the stability of ecosystems1, nutrient cycles2, and 11 global food supplies3 if the processes that produce soil cannot keep pace. Over millennial 12 timescales, the rate of soil production is thought to keep pace with the rate of surface 13 erosion through negative feedbacks between soil thickness and the rate at which soil is 14 produced from the underlying mineral substrate4,5. This paradigm in the Earth Sciences 15 holds that some underlying mechanism lowers the rate of soil production when soil is thick 16 and increases the rate of soil production when soils are thin. This dynamic balance lends 17 support to two observations: First, soil covers >90% of Earth’s ice-free surface (NRCS) 18 despite global erosion rates that vary by three orders of magnitude3 and second, the 19 thickness of soils on Earth exists within a relatively narrow range even in old and deeply 20 weathered landscapes7. However, the actual coupling mechanism between soil thickness 21 and depth is unknown, and the functional form of the relationship is debated. -
Rusell Review
European Journal of Soil Science, March 2019, 70, 216–235 doi: 10.1111/ejss.12790 Rusell Review Pedology and digital soil mapping (DSM) Yuxin Ma , Budiman Minasny , Brendan P. Malone & Alex B. Mcbratney Sydney Institute of Agriculture, School of Life and Environmental Sciences, The University of Sydney, Eveleigh, New South Wales, Australia Summary Pedology focuses on understanding soil genesis in the field and includes soil classification and mapping. Digital soil mapping (DSM) has evolved from traditional soil classification and mapping to the creation and population of spatial soil information systems by using field and laboratory observations coupled with environmental covariates. Pedological knowledge of soil distribution and processes can be useful for digital soil mapping. Conversely, digital soil mapping can bring new insights to pedogenesis, detailed information on vertical and lateral soil variation, and can generate research questions that were not considered in traditional pedology. This review highlights the relevance and synergy of pedology in soil spatial prediction through the expansion of pedological knowledge. We also discuss how DSM can support further advances in pedology through improved representation of spatial soil information. Some major findings of this review are as follows: (a) soil classes can bemapped accurately using DSM, (b) the occurrence and thickness of soil horizons, whole soil profiles and soil parent material can be predicted successfully with DSM techniques, (c) DSM can provide valuable information on pedogenic processes (e.g. addition, removal, transformation and translocation), (d) pedological knowledge can be incorporated into DSM, but DSM can also lead to the discovery of knowledge, and (e) there is the potential to use process-based soil–landscape evolution modelling in DSM. -
Developing Glassy Magnets from Simulated Composition of Moon/Mars Regolith for Exploration Applications
Developing Glassy Magnets from simulated Composition of Moon/Mars Regolith for Exploration Applications C. S. Ray1, N. Ramachandran2 and J. Rogers1 1Exploration Science and Technology Division 2BAE SYSTEMS Analytical Solutions Inc. Science and Technology Directorate NASA Marshall Space Flight Center Huntsville, AL 35812 ABSTRACT The feasibility of preparing glasses and developing glass-ceramic materials that display magnetic characteristics using the simulated compositions of Lunar and Martian regoliths have been demonstrated. The reported results are preliminary at this time, and are part of a larger on- going research activity at the NASA Marshall Space Flight Center (MSFC) with an overall goal aimed at (i) developing glass, ceramic and glass-ceramic type materials from the Lunar and Martian soil compositions in their respective simulated atmospheric conditions, (ii) exploring the potential application areas of these materials through extensive materials characterization, and (iii) further improving the related materials properties through a variation of the processing methods. This research activity is an important component of NASA’s current space exploration program, which encourages feasibility studies for materials development using in situ resources on planetary bodies to meet the technological and scientific needs of future human habitats on these extra terrestrial outposts. This paper presents an overview of this on-going work at NASA (MSFC) and reports on a few selected results obtained to date. INTRODUCTION The long-term space exploration goals of NASA include developing human habitats and conducting scientific investigations on planetary bodies, especially on Moon and Mars. In-situ resource processing and utilization on planetary bodies, therefore, is recognized as an important and integral part of NASA’s space exploration program [1], since it can minimize (or eliminate) the level of up-mass (transporting materials from earth to the planetary bodies) and, hence, can substantially reduce the overall work-load and costs of exploration missions. -
Organic Material on Ceres: Insights from Visible and Infrared Space Observations
life Article Organic Material on Ceres: Insights from Visible and Infrared Space Observations Andrea Raponi 1,* , Maria Cristina De Sanctis 1, Filippo Giacomo Carrozzo 1 , Mauro Ciarniello 1 , Batiste Rousseau 1 , Marco Ferrari 1 , Eleonora Ammannito 2, Simone De Angelis 1, Vassilissa Vinogradoff 3, Julie C. Castillo-Rogez 4, Federico Tosi 1, Alessandro Frigeri 1 , Michelangelo Formisano 1 , Francesca Zambon 1, Carol A. Raymond 4 and Christopher T. Russell 5 1 Istituto Nazionale di Astrofisica–Istituto di Astrofisica e Planetologia Spaziali, 00133 Rome, Italy; [email protected] (M.C.D.S.); fi[email protected] (F.G.C.); [email protected] (M.C.); [email protected] (B.R.); [email protected] (M.F.); [email protected] (S.D.A.); [email protected] (F.T.); [email protected] (A.F.); [email protected] (M.F.); [email protected] (F.Z.) 2 Agenzia Spaziale Italiana, 00133 Rome, Italy; [email protected] 3 Physique des Interactions Ioniques et Moléculaires, PIIM, Université d’Aix-Marseille, 13013 Marseille, France; [email protected] 4 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA; [email protected] (J.C.C.-R.); [email protected] (C.A.R.) 5 Earth Planetary and Space Sciences, University of California, Los Angeles, CA 90095, USA; [email protected] * Correspondence: [email protected] Abstract: The NASA/Dawn mission has acquired unprecedented measurements of the surface of the dwarf planet Ceres, the composition of which is a mixture of ultra-carbonaceous material, phyllosilicates, carbonates, organics, Fe-oxides, and volatiles as determined by remote sensing instruments including the VIR imaging spectrometer. -
Geology of Dwarf Planet Ceres and Meteorite Analogs H
80th Annual Meeting of the Meteoritical Society 2017 (LPI Contrib. No. 1987) 6003.pdf GEOLOGY OF DWARF PLANET CERES AND METEORITE ANALOGS H. Y. McSween1, C. A. Raymond2, T. H. Prettyman3, M. C. De Sanctis4, J. C. Castillo-Rogez2, C. T. Russell5, and the Dawn Science Team, 1Department of Earth & Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, [email protected]. 2Jet Propulsion Laboratory, Pasadena, CA 91109, 3Planetary Science Institute, Tucson, AZ 85719, 4Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy, 5Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA 90095. Introduction: Although no known meteorites are thought to derive from Ceres, CI/CM carbonaceous chondrites are potential analogs for its composition and alteration [1]. These meteorites have primitive chemical compositions, despite having suffered aqueous alteration; this paradox can be explained by closed-system alteration in small parent bodies where low permeability limited fluid transport. In contrast, Ceres, the largest asteroidal body, has experi- enced extensive alteration accompanied by differentiation of silicates and volatiles [2]. The ancient surface of Ceres has a crater density similar to Vesta, but basins >400 km are absent or relaxed. The Dawn spacecraft’s GRaND instrument revealed near-surface ice concentrations in the regolith at high latitudes [3], exposed on the surface locally in a few craters [4]. The VIR instrument indicates a dark surface interpreted as a lag deposit from ice sublimation and composed of ammoniated clays, serpentine, MgCa-carbonates, and a darkening component [5]. Elemental analysis of Fe and H abundances in the non-icy regolith are lower and higher, respective- ly, than for CI/CM chondrites [3].