Origin and Mineralogy of Lunar Meteorites. a Study for Lunar Mining and Resources Exploitation

Total Page:16

File Type:pdf, Size:1020Kb

Origin and Mineralogy of Lunar Meteorites. a Study for Lunar Mining and Resources Exploitation Master in Aerospace Engineering Esther Mas Sanz Origin and mineralogy of Lunar meteorites. A study for lunar mining and resources exploitation Master’s Final Degree Project - Report Director: Dr. Josep M. Trigo-Rodríguez (CSIC-IEEC) Tutor: Dr. Miquel Sureda Anfres (UPC) Course: 2019-2020, Spring Semester Delivery date: 22nd June, 2020 [This page intentionally left blank] Acknowledgements I want to express my gratitude to the director of my Master Thesis, Dr. Josep M. Trigo- Rodríguez, for his support throughout the project and particularly, during the difficult situation we all have lived under the pandemic of covid-19. Despite the limitations this project has been possible, perhaps not as complete as firstly imagined but still, robust and rewarding. Likewise, I thank Dr.Miquel Sureda for promptly solving all of my doubts and the ESEIAAT administration for rapidly adapting the course to the new circumstances. I also appreciate the effort of my family and beloved ones, for making these hard times easier to bear and for their unconditional support. Finally, my most sincere gratitude for all of those who, during the coronavirus crisis, have taken care of the most vulnerable and those who have ensured that the gears of society kept working. Thank you all. Abstract In recent years the Moon has become once again the target for many of the most ambitious space projects. Our satellite is expected to provide a permanent base by 2030s and open new possibilities for deep-space exploration and the conquest of Mars. During this decade it is paramount to expand our knowledge on lunar surface mineralogy, chemistry and geology; to prospect it and lay the foundations for the future exploitation of its resources. Lunar achondrites provide interesting information about the main rock-forming minerals of the Moon. These rocks were excavated and delivered to Earth by continuous collisions going on the surface of our satellite. Unfortunately we do not know the exact region of origin of these rocks, so the information provided is only partial. This Master Thesis will study the physico-chemical properties of Lunar meteorites, and will also study the main dynamic pathways followed by Lunar meteorites reaching planet Earth. I declare that, the work in this Master Thesis is completely my own work, no part of this Master Thesis is taken from other people’s work without giving them credit, all references have been clearly cited, I understand that an infringement of this declaration leaves me subject to the foreseen disciplinary actions by Universitat Politècnica de Catalunya - BarcelonaTECH. Student Name: Signature: Date: Esther Mas Sanz 22nd June, 2020 Title of the Thesis: Origin and mineralogy of Lunar meteorites. A study for lunar mining and resources exploitation. Lunar Meteorites: Origin and Mineralogy CONTENTS Contents List of Figures iii List of Tablesv 1 Introduction4 1.1 The Moon, our closest neighbour ....................... 4 1.1.1 A New Race to the Moon: Lunar Mining ............... 6 1.2 Meteoritics .................................... 8 1.2.1 Meteorite classification ......................... 9 1.2.2 Differentiated Meteorites: Achondrites . 10 1.3 Lunar Meteorites ................................ 11 1.3.1 Lunaites Classification ......................... 12 1.3.2 Recovery Locations ........................... 14 1.4 Lunar Geochemistry .............................. 15 1.4.1 Inorganic constituents in Lunar Soil . 17 1.5 Lunar Ejecta .................................. 20 1.5.1 CREAs ................................. 20 I Mineralogy Study 23 2 Chemical and mineralogical characterization of lunar achondrites 23 2.1 SEM+EDX ................................... 23 2.1.1 Solver for Mineral Proportions ..................... 24 3 Lunar Meteorite Samples 27 3.1 JaH 838 ..................................... 27 3.1.1 SEM/EDX Microscopy Results .................... 29 i Lunar Meteorites: Origin and Mineralogy CONTENTS 3.2 Dho 1084 .................................... 33 3.2.1 SEM/EDX Microscopy Results .................... 34 3.3 NWA 11444 ................................... 37 3.3.1 SEM/EDX Microscopy Results .................... 38 3.4 Results Summary ................................ 45 3.5 Conclusions ................................... 47 II Orbital Dynamics Study 49 4 Introduction 49 4.1 Software and Databases ............................ 49 4.2 Previous Works ................................. 50 5 Simulations of Lunar Ejecta 51 5.1 Short transfers ................................. 54 5.1.1 Variation of launch direction ...................... 54 5.1.2 Variation of Ejection Angle ...................... 66 5.1.3 Variation of Earth-Moon-Sun configuration . 71 5.1.4 Summary of results ........................... 76 5.2 Long transfers .................................. 77 5.2.1 Case study: Meteorite Impact on the Moon . 84 5.2.2 Summary of results ........................... 92 6 Conclusions 93 7 Future Work 96 8 Planning 97 Bibliography 98 ii Lunar Meteorites: Origin and Mineralogy LIST OF FIGURES List of Figures 1.1 Representations of the Moon in prehistory and ancient cultures . 4 1.2 Apollo 17 astronaut collecting samples .................... 5 1.3 Water content on the Moon .......................... 7 1.4 Classification diagram of meteorites [72] ................... 10 1.5 Lunar meteorites recovery sites statistical analysis. Database for analysis can be found in [36] ............................... 14 1.6 Images of the Moon surface .......................... 15 1.7 Examples of geochemical bimodality of pristine non-mare rocks. 17 1.8 Images of metals on the Moon surface ..................... 18 1.9 Images of thorium (correlated to KREEP) on the Moon surface . 18 1.10 Cumulative percentage impacted with Earth . 22 2.1 Energy dispersive X-ray spectrum ....................... 24 2.2 Ternary diagram of of the composition of feldspar minerals. 25 3.1 Location of the JaH 838 meteorite ....................... 27 3.2 Mosaic of JaH 838 ............................... 29 3.3 Meteorite JaH 838 ROIs ............................ 30 3.4 Spectrum 6 JaH 838 .............................. 30 3.5 SEM/EDX mapping of JaH 838 ........................ 32 3.6 Location of the Dho 1084 meteorite ...................... 33 3.7 Mosaic of DHO 1084 .............................. 34 3.8 Meteorite DHO 1084 ROI ........................... 35 3.9 Spectrum 3 of the mapping of DHO 1084 ................... 36 3.10 Mosaic of NWA 11444 ............................. 38 3.11 ROIs of NWA 11444 .............................. 39 3.12 Spectrum 3 of the mapping of NWA 11444 (ROI 1) . 40 iii Lunar Meteorites: Origin and Mineralogy LIST OF FIGURES 3.13 Spectrum 1 of the mapping of NWA 11444, ROI 2 . 41 3.14 Spectrum 1 of the mapping of NWA 11444 (ROI 3) . 43 3.15 SEM/EDX mapping of NWA 11444 ...................... 44 5.1 Moon Launching Sites ............................. 51 5.2 Launching sites and velocities for different directions of launch and ejection angles ...................................... 52 5.3 Moon coordinates ................................ 53 5.4 Velocity vectors in mooncentric and geocentric orbits . 53 5.5 Variation of Earth impacts with launch velocity . 58 5.6 Trajectories of two particles in geocentric orbits . 59 5.7 Evolution of the meteoroid impact population . 60 5.8 Evolution of the meteoroid impact population (logarithmic scale) . 61 5.9 Launch angle of particles according to their launch site. 62 5.10 Correlation between launch site and Earth collisions with varying launch direction ..................................... 63 5.11 Correlation between launch site and Earth collisions with varying launch direction at different times. ........................... 64 5.12 Histogram of Earth Impacts as function of ejection angle and ejection velocity 67 5.13 Flat view of the four histograms for Earth Impacts as function of ejection angle and ejection velocity ........................... 67 5.14 Comparison between ejection angles ...................... 69 5.15 Launch angle of particles according to their launch site . 70 5.16 Different Earth-Moon-Sun configurations for lunar ejecta launches . 72 5.17 Earth impacts for different velocities and initial dates . 73 5.18 Minimum time for a lunar ejecta to impact with Earth (histogram) . 75 5.19 Minimum time for a lunar ejecta to impact with Earth . 75 5.20 Evolution of launch angles for long time scales. 78 5.21 Initial orbital elements. ............................. 79 5.22 Final orbital elements. ............................. 79 5.23 Semi-major axis vs. eccentricity evolution in time . 80 5.24 Lunar ejecta survivor population after 105 years. 81 iv Lunar Meteorites: Origin and Mineralogy LIST OF TABLES 5.25 Accumulated impacts % ............................ 83 5.27 Detailed map of the Moon surface. ...................... 85 5.28 Impact point and directions of launch for the lunar ejecta. 86 5.29 Distribution of lunar ejecta after 104 years. 86 5.30 Orbital elements at collision instant. ..................... 87 5.31 Orbital elements at collision instant. ..................... 88 5.32 Orbital elements evolution of M184. ...................... 89 5.33 Time evolution of the orbital elements for different ejected particles. 90 5.34 Histogram of Earth collisions. ......................... 91 8.1 Gantt Diagram. ................................. 97 List of Tables 1.1 Denomination of object and phenomena according to diameter range. See [71], [70], [72]. .................................. 9 1.2 Main mineral components found in meteorites [73].
Recommended publications
  • The Surrender Software
    Scientific image rendering for space scenes with the SurRender software Scientific image rendering for space scenes with the SurRender software R. Brochard, J. Lebreton*, C. Robin, K. Kanani, G. Jonniaux, A. Masson, N. Despré, A. Berjaoui Airbus Defence and Space, 31 rue des Cosmonautes, 31402 Toulouse Cedex, France [email protected] *Corresponding Author Abstract The autonomy of spacecrafts can advantageously be enhanced by vision-based navigation (VBN) techniques. Applications range from manoeuvers around Solar System objects and landing on planetary surfaces, to in -orbit servicing or space debris removal, and even ground imaging. The development and validation of VBN algorithms for space exploration missions relies on the availability of physically accurate relevant images. Yet archival data from past missions can rarely serve this purpose and acquiring new data is often costly. Airbus has developed the image rendering software SurRender, which addresses the specific challenges of realistic image simulation with high level of representativeness for space scenes. In this paper we introduce the software SurRender and how its unique capabilities have proved successful for a variety of applications. Images are rendered by raytracing, which implements the physical principles of geometrical light propagation. Images are rendered in physical units using a macroscopic instrument model and scene objects reflectance functions. It is specially optimized for space scenes, with huge distances between objects and scenes up to Solar System size. Raytracing conveniently tackles some important effects for VBN algorithms: image quality, eclipses, secondary illumination, subpixel limb imaging, etc. From a user standpoint, a simulation is easily setup using the available interfaces (MATLAB/Simulink, Python, and more) by specifying the position of the bodies (Sun, planets, satellites, …) over time, complex 3D shapes and material surface properties, before positioning the camera.
    [Show full text]
  • South Pole-Aitken Basin: Crater Size-Frequency Distribution Measurements
    EPSC Abstracts Vol. 7 EPSC2012-832 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 South Pole-Aitken Basin: Crater Size-Frequency Distribution Measurements H. Hiesinger1, C. H. van der Bogert1, J. H. Pasckert1, N. Schmedemann2, M.S. Robinson3, B. Jolliff4, and N. Petro5; 1Institut für Planetologie (IfP), WWU Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany ([email protected]/ +49-251-8339057), 2Institute of Geosciences, Freie Universität Berlin, Germany, 3Arizona State University, Tempe, USA, 4Dept. of Earth and Planet. Sci. Washington Univ., St. Louis, USA, 5Goddard Spaceflight Center, Greenbelt, USA. Introduction morphology and topography derived from the LROC Being the largest basin (>2500 km in diameter) WAC mosaic and LOLA. LOLA topography was and presumably the oldest preserved impact structure also used to identify old and highly degraded impact on the Moon [e.g., 1], the South Pole-Aitken (SPA) structures and to improve our statistics in areas with basin is of particular interest. SPA might have large shadows close to the pole. The CSFDs were penetrated the entire lunar crust and exposed lower plotted with CraterStats [7], applying the lunar crustal or upper mantle material, but despite its deep chronology (CF) of [8] and the production function penetration, it did not reveal KREEP-rich rocks in (PF) of [9]. From this we derived absolute model contrast with the Imbrium basin. In addition, its age ages (AMAs) for craters between ~1.5 km and 300 should shed light on the plausibility of the terminal km in diameter [9]. More details on the technique of cataclysm [e.g., 2].
    [Show full text]
  • Monte Carlo Methods to Calculate Impact Probabilities⋆
    A&A 569, A47 (2014) Astronomy DOI: 10.1051/0004-6361/201423966 & c ESO 2014 Astrophysics Monte Carlo methods to calculate impact probabilities? H. Rickman1;2, T. Wisniowski´ 1, P. Wajer1, R. Gabryszewski1, and G. B. Valsecchi3;4 1 P.A.S. Space Research Center, Bartycka 18A, 00-716 Warszawa, Poland e-mail: [email protected] 2 Dept. of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden 3 IAPS-INAF, via Fosso del Cavaliere 100, 00133 Roma, Italy 4 IFAC-CNR, via Madonna del Piano 10, 50019 Sesto Fiorentino (FI), Italy Received 9 April 2014 / Accepted 28 June 2014 ABSTRACT Context. Unraveling the events that took place in the solar system during the period known as the late heavy bombardment requires the interpretation of the cratered surfaces of the Moon and terrestrial planets. This, in turn, requires good estimates of the statistical impact probabilities for different source populations of projectiles, a subject that has received relatively little attention, since the works of Öpik(1951, Proc. R. Irish Acad. Sect. A, 54, 165) and Wetherill(1967, J. Geophys. Res., 72, 2429). Aims. We aim to work around the limitations of the Öpik and Wetherill formulae, which are caused by singularities due to zero denominators under special circumstances. Using modern computers, it is possible to make good estimates of impact probabilities by means of Monte Carlo simulations, and in this work, we explore the available options. Methods. We describe three basic methods to derive the average impact probability for a projectile with a given semi-major axis, eccentricity, and inclination with respect to a target planet on an elliptic orbit.
    [Show full text]
  • Warren and Taylor-2014-In Tog-The Moon-'Author's Personal Copy'.Pdf
    This article was originally published in Treatise on Geochemistry, Second Edition published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non- commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Warren P.H., and Taylor G.J. (2014) The Moon. In: Holland H.D. and Turekian K.K. (eds.) Treatise on Geochemistry, Second Edition, vol. 2, pp. 213-250. Oxford: Elsevier. © 2014 Elsevier Ltd. All rights reserved. Author's personal copy 2.9 The Moon PH Warren, University of California, Los Angeles, CA, USA GJ Taylor, University of Hawai‘i, Honolulu, HI, USA ã 2014 Elsevier Ltd. All rights reserved. This article is a revision of the previous edition article by P. H. Warren, volume 1, pp. 559–599, © 2003, Elsevier Ltd. 2.9.1 Introduction: The Lunar Context 213 2.9.2 The Lunar Geochemical Database 214 2.9.2.1 Artificially Acquired Samples 214 2.9.2.2 Lunar Meteorites 214 2.9.2.3 Remote-Sensing Data 215 2.9.3 Mare Volcanism
    [Show full text]
  • Can Moons Have Moons?
    A MNRAS 000, 1–?? (2018) Preprint 23 January 2019 Compiled using MNRAS L TEX style file v3.0 Can Moons Have Moons? Juna A. Kollmeier1⋆ & Sean N. Raymond2† 1 Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 2 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, all´eGeoffroy Saint-Hilaire, 33615 Pessac, France Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Each of the giant planets within the Solar System has large moons but none of these moons have their own moons (which we call submoons). By analogy with studies of moons around short-period exoplanets, we investigate the tidal-dynamical stability of submoons. We find that 10 km-scale submoons can only survive around large (1000 km-scale) moons on wide-separation orbits. Tidal dissipation destabilizes the orbits of submoons around moons that are small or too close to their host planet; this is the case for most of the Solar System’s moons. A handful of known moons are, however, capable of hosting long-lived submoons: Saturn’s moons Titan and Iapetus, Jupiter’s moon Callisto, and Earth’s Moon. Based on its inferred mass and orbital separation, the newly-discovered exomoon candidate Kepler-1625b-I can in principle host a large submoon, although its stability depends on a number of unknown parameters. We discuss the possible habitability of submoons and the potential for subsubmoons. The existence, or lack thereof, of submoons, may yield important constraints on satellite formation and evolution in planetary systems. Key words: planets and satellites – exoplanets – tides 1 INTRODUCTION the planet spins quickly or to shrink if the planet spins slowly (e.g.
    [Show full text]
  • Constraints on the Habitability of Extrasolar Moons 3 ¯Glob Its Orbit-Averaged Global Energy flux Fs
    Formation, detection, and characterization of extrasolar habitable planets Proceedings IAU Symposium No. 293, 2012 c 2012 International Astronomical Union Nader Haghighipour DOI: 00.0000/X000000000000000X Constraints on the habitability of extrasolar moons Ren´eHeller1 and Rory Barnes2,3 1Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam email: [email protected] 2University of Washington, Dept. of Astronomy, Seattle, WA 98195, USA 3Virtual Planetary Laboratory, NASA, USA email: [email protected] Abstract. Detections of massive extrasolar moons are shown feasible with the Kepler space telescope. Kepler’s findings of about 50 exoplanets in the stellar habitable zone naturally make us wonder about the habitability of their hypothetical moons. Illumination from the planet, eclipses, tidal heating, and tidal locking distinguish remote characterization of exomoons from that of exoplanets. We show how evaluation of an exomoon’s habitability is possible based on the parameters accessible by current and near-future technology. Keywords. celestial mechanics – planets and satellites: general – astrobiology – eclipses 1. Introduction The possible discovery of inhabited exoplanets has motivated considerable efforts towards estimating planetary habitability. Effects of stellar radiation (Kasting et al. 1993; Selsis et al. 2007), planetary spin (Williams & Kasting 1997; Spiegel et al. 2009), tidal evolution (Jackson et al. 2008; Barnes et al. 2009; Heller et al. 2011), and composition (Raymond et al. 2006; Bond et al. 2010) have been studied. Meanwhile, Kepler’s high precision has opened the possibility of detecting extrasolar moons (Kipping et al. 2009; Tusnski & Valio 2011) and the first dedicated searches for moons in the Kepler data are underway (Kipping et al.
    [Show full text]
  • Moon Minerals a Visual Guide
    Moon Minerals a visual guide A.G. Tindle and M. Anand Preliminaries Section 1 Preface Virtual microscope work at the Open University began in 1993 meteorites, Martian meteorites and most recently over 500 virtual and has culminated in the on-line collection of over 1000 microscopes of Apollo samples. samples available via the virtual microscope website (here). Early days were spent using LEGO robots to automate a rotating microscope stage thanks to the efforts of our colleague Peter Whalley (now deceased). This automation speeded up image capture and allowed us to take the thousands of photographs needed to make sizeable (Earth-based) virtual microscope collections. Virtual microscope methods are ideal for bringing rare and often unique samples to a wide audience so we were not surprised when 10 years ago we were approached by the UK Science and Technology Facilities Council who asked us to prepare a virtual collection of the 12 Moon rocks they loaned out to schools and universities. This would turn out to be one of many collections built using extra-terrestrial material. The major part of our extra-terrestrial work is web-based and we The authors - Mahesh Anand (left) and Andy Tindle (middle) with colleague have build collections of Europlanet meteorites, UK and Irish Peter Whalley (right). Thank you Peter for your pioneering contribution to the Virtual Microscope project. We could not have produced this book without your earlier efforts. 2 Moon Minerals is our latest output. We see it as a companion volume to Moon Rocks. Members of staff
    [Show full text]
  • Lunar Meteorites: Impact Melt and Regolith Breccias and Large-Scale Heterogeneities of the Upper Lunar Crust
    Meteoritics & Planetary Science 40, Nr 7, 989–1014 (2005) Abstract available online at http://meteoritics.org “New” lunar meteorites: Impact melt and regolith breccias and large-scale heterogeneities of the upper lunar crust Paul H. WARREN*, Finn ULFF-MØLLER, and Gregory W. KALLEMEYN Institute of Geophysics, University of California—Los Angeles, Los Angeles, California 90095–1567, USA *Corresponding author. E-mail: [email protected] (Received 06 May 2002; revision accepted 24 April 2005) Abstract–We have analyzed nine highland lunar meteorites (lunaites) using mainly INAA. Several of these rocks are difficult to classify. Dhofar 081 is basically a fragmental breccia, but much of its groundmass features a glassy-fluidized texture that is indicative of localized shock melting. Also, much of the matrix glass is swirly-brown, suggesting a possible regolith derivation. We interpret Dar al Gani (DaG) 400 as an extremely immature regolith breccia consisting mainly of impact-melt breccia clasts; we interpret Dhofar 026 as an unusually complex anorthositic impact-melt breccia with scattered ovoid globules that formed as clasts of mafic, subophitic impact melt. The presence of mafic crystalline globules in a lunar material, even one so clearly impact-heated, suggests that it may have originated as a regolith. Our new data and a synthesis of literature data suggest a contrast in Al2O3- incompatible element systematics between impact melts from the central nearside highlands, where Apollo sampling occurred, and those from the general highland surface of the Moon. Impact melts from the general highland surface tend to have systematically lower incompatible element concentration at any given Al2O3 concentration than those from Apollo 16.
    [Show full text]
  • "Ringing" from an Asteroid Collision Event Which Triggered the Flood?
    The Proceedings of the International Conference on Creationism Volume 6 Print Reference: Pages 255-261 Article 23 2008 Is the Moon's Orbit "Ringing" from an Asteroid Collision Event which Triggered the Flood? Ronald G. Samec Bob Jones University Follow this and additional works at: https://digitalcommons.cedarville.edu/icc_proceedings DigitalCommons@Cedarville provides a publication platform for fully open access journals, which means that all articles are available on the Internet to all users immediately upon publication. However, the opinions and sentiments expressed by the authors of articles published in our journals do not necessarily indicate the endorsement or reflect the views of DigitalCommons@Cedarville, the Centennial Library, or Cedarville University and its employees. The authors are solely responsible for the content of their work. Please address questions to [email protected]. Browse the contents of this volume of The Proceedings of the International Conference on Creationism. Recommended Citation Samec, Ronald G. (2008) "Is the Moon's Orbit "Ringing" from an Asteroid Collision Event which Triggered the Flood?," The Proceedings of the International Conference on Creationism: Vol. 6 , Article 23. Available at: https://digitalcommons.cedarville.edu/icc_proceedings/vol6/iss1/23 In A. A. Snelling (Ed.) (2008). Proceedings of the Sixth International Conference on Creationism (pp. 255–261). Pittsburgh, PA: Creation Science Fellowship and Dallas, TX: Institute for Creation Research. Is the Moon’s Orbit “Ringing” from an Asteroid Collision Event which Triggered the Flood? Ronald G. Samec, Ph. D., M. A., B. A., Physics Department, Bob Jones University, Greenville, SC 29614 Abstract We use ordinary Newtonian orbital mechanics to explore the possibility that near side lunar maria are giant impact basins left over from a catastrophic impact event that caused the present orbital configuration of the moon.
    [Show full text]
  • NWA 5000 – ONE of a KIND? N. Artemieva1,2. 1Planetary Science Institute, [email protected]
    77th Annual Meteoritical Society Meeting (2014) 5231.pdf NWA 5000 – ONE OF A KIND? N. Artemieva1,2. 1Planetary Science Institute, [email protected]. 2Instiitute for Dynamics of Geospheres, RAS, Russia. Introduction: The list of lunar meteorites consists of 95 names with the total mass of ~75 kg. The spallation theory [1] and numerical simulations [2-4] allowed to explain the formation of solid high-velocity ejecta and to reconcile the results of nu- merical models with observations. Presence of a porous regolith layer on the Moon decreases at least tenfold the total mass of sol- id escape ejecta because of much lower shock pressures required for shock melting [4]. Projectiles smaller than 10-20 m in diame- ter are able to propel exclusively the regolith (i.e., molten dust with random and unknown inclusions of consolidated breccia or rocks) into space. It means that the contribution of these small cratering events to the flux of lunar meteorites is non-predictable. Larger impact events which are able to excavate underlying megaregolith are statistically unlikely within a short, < 10 kyr, time frame [5]. Thus, one of the biggest (11.5 kg) and the young- est (terrestrial age <10 kyr, [6]) lunar meteorite, NWA 5000 (feldsparic breccia) is a real miracle. Numerical model and initial conditions: High-velocity im- pacts on the Moon are modeled using the 3D hydrocode SOVA [7] complemented by the ANEOS equation of state for geological materials. The lunar regolith porosity is described in the frame of ε-alpha model [8]. Tracer particles are used to find dynamics and thermal history of solid inclusions into the regolith.
    [Show full text]
  • ELEMENTAL ABUNDANCES in the SILICATE PHASE of PALLASITIC METEORITES Redacted for Privacy Abstract Approved: Roman A
    AN ABSTRACT OF THE THESIS OF THURMAN DALE COOPER for theMASTER OF SCIENCE (Name) (Degree) in CHEMISTRY presented on June 1, 1973 (Major) (Date) Title: ELEMENTAL ABUNDANCES IN THE SILICATE PHASE OF PALLASITIC METEORITES Redacted for privacy Abstract approved: Roman A. Schmitt The silicate phases of 11 pallasites were analyzed instrumen- tally to determine the concentrations of some major, minor, and trace elements.The silicate phases were found to contain about 98% olivine with 1 to 2% accessory minerals such as lawrencite, schreibersite, troilite, chromite, and farringtonite present.The trace element concentrations, except Sc and Mn, were found to be extremely low and were found primarily in the accessory phases rather than in the pure olivine.An unusual bimodal Mn distribution was noted in the pallasites, and Eagle Station had a chondritic nor- malized REE pattern enrichedin the heavy REE. The silicate phases of pallasites and mesosiderites were shown to be sufficiently diverse in origin such that separate classifications are entirely justified. APPROVED: Redacted for privacy Professor of Chemistry in charge of major Redacted for privacy Chairman of Department of Chemistry Redacted for privacy Dean of Graduate School Date thesis is presented June 1,1973 Typed by Opal Grossnicklaus for Thurman Dale Cooper Elemental Abundances in the Silicate Phase of Pallasitic Meteorites by Thurman Dale Cooper A THESIS submitted to Oregon State University in partial fulfillment of the requirements for the degree of Master of Science June 1974 ACKNOWLEDGMENTS The author wishes to express his gratitude to Prof. Roman A. Schmitt for his guidance, suggestions, discussions, and thoughtful- ness which have served as an inspiration.
    [Show full text]
  • Journal of Physics Special Topics an Undergraduate Physics Journal
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by University of Leicester Open Journals Journal of Physics Special Topics An undergraduate physics journal P5 1 Conditions for Lunar-stationary Satellites Clear, H; Evan, D; McGilvray, G; Turner, E Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH November 5, 2018 Abstract This paper will explore what size and mass of a Moon-like body would have to be to have a Hill Sphere that would allow for lunar-stationary satellites to exist in a stable orbit. The radius of this body would have to be at least 2500 km, and the mass would have to be at least 2:1 × 1023 kg. Introduction orbital period of 27 days. We can calculate the Geostationary satellites are commonplace orbital radius of the satellite using the following around the Earth. They are useful in provid- equation [3]: ing line of sight over the entire planet, excluding p 3 the polar regions [1]. Due to the Earth's gravi- T = 2π r =GMm; (1) tational influence, lunar-stationary satellites are In equation 1, r is the orbital radius, G is impossible, as the Moon's smaller size means it the gravitational constant, MM is the mass of has a small Hill Sphere [2]. This paper will ex- the Moon, and T is the orbital period. Solving plore how big the Moon would have to be to allow for r gives a radius of around 88000 km. When for lunar-stationary satellites to orbit it.
    [Show full text]