DOCSLIB.ORG

IMPACT CRATERING: the EFFECTS of TARGET TOPOGRAPHY and HETEROGENEITY Submitted to NASA Research Announcement NNH15ZDA001N-SSW, Solar System Workings

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
IMPACT CRATERING: the EFFECTS of TARGET TOPOGRAPHY and HETEROGENEITY Submitted to NASA Research Announcement NNH15ZDA001N-SSW, Solar System Workings $ + 2 3 +#> 7 !"!## *+$% &'&( ')($ *+',))--)&'.-' (*)''.%.*( %,/ 0,)')(.*) )$'/ SECTION VII - Project Summary $ '(.0#&'$. +$8B;; 9A < ; <A 88; ;B; ;B ; A8C 7 6 < A 6 7 8$8B; 8; A; < ;B < 4D;>9 < ;8 6 B 9 A; 49 9 8D9A 96A4 6;A9 8 & 6 9 AD;> 8 ; 8B;; 8DB 8 8 ;68 6 68 B 8 67; 64A89 4 86767 9 'A 4D 9DB 8 8 ;68 69B > 67 9 ;A; 9 A ; 8B; 6 ;> 8+ 9A A;< A 9 ; BA 96 A ; &$) &)*. 0.@)&'$E)+'A96 A B B AD69;6 BDB 868B; ; 9 <7> 99A ; 96 9B9 BA7 9AA 97A8B;B ; $ B ;6 466 7AA > <6 ;AD;> 8 6 89 98B;; 4A9 A 8 ; A; AB4 A 6; 8 BA8 766 A 6 B 8 7D 9; ;69 6 AB ; <A<A> ;A;8B6D 9 )',.0..*/+$8B;; 9DB 8 66<B 8 A)DB 86$8B;< 7 A B;& '> >DB 86;A: 66< < >A; 9B ; 68FA)C; E6;7 87 8G)EH (6'8% 697 8G('%H'A)EB C; > ;66 B6A 9A A8B;B B B ;6 A 9 ;'A 6 B6 < A6&&0;8 89 A>4A;A66 > 6C;B ;6 < ; 69A <66 ; C; 8AB ;6I C; B 4 B 4 96'A('%B C; 6 B6> ;667A 9 ;668; ;A 9AA 9 98B;; 4A;A A89 <7> ;8 'A 66 A; B 6< ; 9; D;>4 9 A4 8 ;@A A ;A: 66B > 9AA ; 9B9 BA7 A 97A A9A67 78;B ; ; D;>49 A4 8 ; 206 ; 66< 8; AB 8 A <8668 B ; ())E &)+$8B;; 9 8C B ; ;9B6 7 ; 66 ;6 A 9A8A 6 7 8 'ADB 86 A B ; 8B;; 9 9B9 BA7 A 97B B A 6> 6 7 8 9 8 AJ>6 8 ; ; KG BB D&2H 12<4<%/""= /6" "> IMPACT CRATERING: THE EFFECTS OF TARGET TOPOGRAPHY AND HETEROGENEITY Submitted to NASA Research Announcement NNH15ZDA001N-SSW, Solar System Workings Principal Investigator: Jennifer L. B. Anderson (Winona State University) Co-Investigator: Mark J. Cintala (NASA Johnson Space Center) Collaborator: Jeffrey Plescia (Johns Hopkins Applied Physics Lab) CONTENTS 1 SCIENTIFIC/TECHNICAL/MANAGEMENT 1.1 Introduction and Implications ……..………………………………………………………………………. 1 1.2 Objectives …………………………………………………………………………………………….……………… 2 1.3 Background ……..………………………………………………………………………………………….………. 2 1.4 Technical Approach & Methodology ……………………………….………….……………….……….. 4 1.4.1 Laboratory Techniques …………………………………………………………………….………. 5 1.4.2 Experiment Design ……………………………….………………………………………….………. 7 1.4.3 Task 1: Effects of Topography ………………….…………………………………………………. 8 1.4.4 Task 2: Effects of Target Heterogeneity …………………………………………………… 9 1.4.5 Dimensionless Scaling Relationships .…….………………………………………………… 11 1.4.6 Application to Lunar Crater Morphology ………….……………………………………… 12 1.4.7 Proof-of-Concept: Target Topography .…….…………..………………………………… 12 1.5 Relevance to NASA and the Solar System Workings Program ……………….……….……. 14 1.6 Work Plan and Schedule …..…………….………………………………………………………….………. 14 1.7 Roles and Responsibilities ………..……………………………………………….………………….……. 14 1.8 Data Management Plan ……………..………………………………………………………………….……. 15 2 REFERENCES ………………………………………………….…………………………………………………………………… 16 3 BIOGRAPHICAL SKETCHES …………………………………………………………………………………………………… 19 4 CURRENT AND PENDING SUPPORT ………………………………………………………………………………….… 23 5 LETTER OF SUPPORT FROM NASA … ………………………………………………………………………………… 26 6 FACILITIES AND EQUIPMENT …………………………………………………………………………………………….. 27 7 BUDGET JUSTIFICATION 7.1 Table of Personnel and Work Effort ……..………………………………………………………………. 28 7.2 Winona State University Budget Narrative and Details …….……………………………… 28 7.3 NASA Johnson Space Center Budget Narrative and Details ……….…………………….…. 31 IMPACT CRATERING: THE EFFECTS OF TARGET TOPOGRAPHY AND HETEROGENEITY – J.L.B. ANDERSON, PI 1 SCIENTIFIC/TECHNICAL/MANAGEMENT 1.1 Introduction and Implications Impact cratering is a fundamental physical process that has dominated the evolution and modification of every planetary surface in the Solar System. Impact craters act as probes of a planetary surface, excavating subsurface material and depositing it outside of the crater, generating and mixing the regolith on airless bodies, and launching future meteorites off a surface. In order to capitalize on the utility of impact craters as a means of probing a planet’s surface, it is important to improve our understanding of the impact-cratering process itself. High- speed accelerators have been used for decades to investigate the impact process in a controlled laboratory environment. New experimental methods allow more quantitative and higher- resolution studies than ever before, illuminating the dynamics of the excavation and modification of growing impact craters in real time [Cintala et al., 1999; Anderson et al., 2003; Barnouin-Jha et al., 2007]. The work proposed here seeks to expand our understanding of the impact cratering process by using these quantitative experimental methods to examine more realistic models of planetary surfaces in the laboratory. Well-defined scaling relationships [e.g., Chabai, 1965; Holsapple and Schmidt, 1982; Housen et al., 1983; Housen and Holsapple, 2011] can then be used to extrapolate the laboratory results to planetary surfaces allowing the application of experimental results to crater morphology on the Moon, Mercury, and asteroids. Current knowledge of the excavation and modification of impact craters from experiments and numerical models is limited primarily to cases of flat, homogeneous, and uniformly layered targets. The only experiments in granular material with any kind of topography known to us were intended to examine the effects of target curvature during very large impacts on spherical bodies [Schultz et al., 1986; Schultz, 1988]. Recently, the first preliminary report of numerically modeled impacts into sloped topography has concluded that the distribution of material ejected during impacts is significantly affected by topography [Elbeshausen and Wünnemann, 2011]. Impact crater morphology and morphometry have been linked to the thickness of a clastic layer (the regolith) on top of a more competent rock unit (typically basalts) on the lunar surface by Oberbeck and Quaide [1968]. Gault et al. [1968] experimentally investigated the effects of interbedded competent and incompetent strata on subsurface crater structure. Numerical simulations have explored layered targets [Senft & Stewart, 2007] and Bart et al. [2011] and Bart [2014] have tested these models using lunar craters. Schultz [2000, 2007] performed experiments into low-impedance layers on top of solid targets to investigate the extent to which such layers can minimize the damage in the underlying competent substrate; similar experiments were performed by Dohi et al. [2012]. Beyond these examples, the added complexities of heterogeneous targets or targets with regional surface topography have not yet been investigated with the goal of applying results to crater-scaling relationships. Thus, existing experimental data and numerical modeling results provide only first-order guidance when considering the effects of impact in a realistic planetary context: rough terrain that can be as heterogeneous in structure at depth as it is irregular at the surface. The goal of the proposed work is to take the next logical step in experimental cratering studies by investigating the effects of target topography and subsurface heterogeneity on the impact PAGE | 1 IMPACT CRATERING: THE EFFECTS OF TARGET TOPOGRAPHY AND HETEROGENEITY – J.L.B. ANDERSON, PI process. In particular, we will identify how these variables affect the excavation of material from a growing impact crater, the growth and modification of the crater shape, and the redistribution of ejected material. We will use a combination of laser illumination and high-speed photography of impact experiments in targets with topographic or subsurface structures similar to those expected on actual planetary surfaces to follow the excavation and modification of growing craters in real time. Experimental data will be used to establish criteria that will guide the interpretation of a cratered surface, specifically those on airless bodies such as the Moon, Mercury, and asteroids with topographic terrains and strength-layered substrates. 1.2 Objectives ¾ To design a variety of simple targets for use in impact experiments that more realistically approximate sloping topography and strength-layered subsurface heterogeneities as expected on planetary surfaces. ¾ To use these targets in impact experiments to examine the effects of topography and target heterogeneity on impact-crater excavation, growth, and modification through the use of a high-resolution ejecta-particle tracking system, a real-time crater-cavity profiling system, and three-dimensional measurements of final crater morphometries. ¾ To modify existing scaling relationships to accommodate the effects of regional topography and subsurface layering and to apply our findings to the interpretation of simple craters on planetary surfaces, specifically the Moon. 1.3 Background Studying the impact-cratering process is challenging for a number of reasons. The events in question are very large, energetic, and (luckily) not common in recent times on the Earth’s surface, so we have very little experience in observing the natural process itself. The Moon has been an enormous resource for morphological and morphometric data about impact craters and has guided our current best understanding of their formation. Field geology at terrestrial craters has allowed us to examine the three-dimensional structure of impact craters and further illuminate the cratering process. The use of accelerators in the laboratory has allowed variables affecting the impact-cratering process to be controlled and the mechanics of formation to be studied in detail at small scales. These experimental results can be scaled to planetary-sized impacts using well-developed, non-dimensional relationships. Mathematical models using first
Load more

Recommended publications
  • Compositional Diversity Inside Lowell Crater, Orientale Basin: Evidences for Extensive Spinel Rich Deposits
    Second Conference on the Lunar Highlands Crust (2012) 9016.pdf COMPOSITIONAL DIVERSITY INSIDE LOWELL CRATER, ORIENTALE BASIN: EVIDENCES FOR EXTENSIVE SPINEL RICH DEPOSITS. N. Srivastava1 and R. P. Gupta2, 1PLANEX, Physical Research Laboratory, Ahmedabad, India – 380009, [email protected], 2Earth Sciences, IIT Roorkee, Roorkee, Uttarakhand, India – 247667, [email protected]. Introduction: Spinel dominant rock exposures de- void of mafic minerals such as olivine and pyroxenes, have been recently found in certain areas both on the far-side and on the near-side of the Moon using data from NASA’s Moon Mineral Mapper (M3) onboard Chandrayaan-1, India’s first mission to the Moon [1, 2]. These include, far-side exposures along the ring of Moscoviense basin, where they were first reported [3] and several near-side exposures such as the extensive occurrences in Sinu Aestuum, in the Theophilus crater, Copernicus crater floor and few exposures in the Tycho crater [4-9]. The mode of formation of this newly discovered rock type on Moon is not clearly understood in the current perspective about the evolu- tion of Moon. Except for Tycho crater, all the above mentioned exposures are found in similar geologic Figure 1: Clementine albedo image showing the re- settings i.e., along the rings of major basins. Hence it gional geologic setting of Lowell crater. is envisaged that most of these rock exposures consti- Methodology: The composition of the exposures tute previously deep-seated rocks which have been in the region have been identified on the basis of char- exhumed on to the surface due to impacts.
    [Show full text]
  • N91"20002 LPSC XXII Press Abst 23
    N91"20002 LPSC XXII Press Abst 23 ORIENTALE AND SOUTH POLE-AITKEN BASINS ON THE MOON: PRELIMINARY GALILEO IMAGING RESULTS. J. Head, E. Fischer, S. Murchie, C. Pieters, J. Plutchak, J. Sunshine (Brown University, Providence, R.I, U.S.A. ); M. Belton (Kitt Peak Nat. Observatory, Tucson, AZ, U.S.A.); M. Cart (USGS, Menlo Park, CA, U.S.A.); C. Chapman (Planetary Science Institute, Tucson, AZ, U.S.A.); M. Davies (RAND, Santa Monica, CA, U.S.A.); F. Fanale, M. Robinson (University of Hawaii, Honolulu, HI, U.S.A.); R. Greeley, R. Sullivan (Arizona State University, Tempe, AZ, U.S.A.); R. Greenberg (University of Arizona, Tucson, AZ, U.S.A.); P. Helfenstein, J. Veverka (Comell University, Ithaca, NY, U.S.A.); H. Hoffmann, R. Jaumann, G. Neukum (DLR, Oberpfaffenhofen, F.R.G.); T, Johnson, K. Klaascn (JPL, Pasadena, CA, U.S.A.); A. McEwen, T. Becker (USGS, Flagstaff, AZ, U.S.A.); C. Pilcher (NASA Headquarters, Washington, D.C., U.S.A.). On the near side of the Moon visible from Earth, the bright areas or "highlands" are composed of light-colored rock saturated with craters formed over eons by impacting meteors. Younger, less cratered, darker plains, or "mare," are composed of a thin layer of basaltic lava flows that erupted over 3 billion years ago and buried highlands-type rocks. The mare plains are concentrated into discrete, circular, topographically low regions called "basins," each of which typically also contains several concentric, ring-like belts of high mountains. Several dozen of these basins, from 300 to nearly 2000 kilometers in diameter, are filled to varying degrees with mare basalts [I,2].
    [Show full text]
  • Origin of the Anomalously Rocky Appearance of Tsiolkovskiy Crater
    Icarus 273 (2016) 237–247 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Origin of the anomalously rocky appearance of Tsiolkovskiy crater ∗ Benjamin T. Greenhagen a, , Catherine D. Neish b, Jean-Pierre Williams c, Joshua T.S. Cahill a, Rebecca R. Ghent d,e,PaulO. Hayne f, Samuel J. Lawrence g,NoahE. Petro h, Joshua L. Bandfield i a Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723-6099, United States b Department of Earth Sciences, Western University Biological & Geological Sciences Building, Room 1026 1151 Richmond St. N. London, ON N6A 5B7 Canada c Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles 595 Charles Young Drive East, Box 951567 Los Angeles, CA 90095-1567, United States d Department of Earth Sciences, Earth Sciences Centre 22 Russell Street Toronto, Ontario, M5S 3B1, Canada e Planetary Science Institute, 1700 East Fort Lowell, Suite 106 Tucson, AZ 85719-2395, United States f Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive Pasadena, CA 91109 ASU, United States g School of Earth and Space Exploration, PO Box 871404 Tempe, AZ 85287-1404, United States h NASA’s Goddard Space Flight Center, 8800 Greenbelt Rd Greenbelt, MD 20771, United States i Space Science Institute, 4750 Walnut Street | Suite 205 Boulder, Colorado 80301, United States a r t i c l e i n f o a b s t r a c t Article history: Rock abundance maps derived from the Diviner Lunar Radiometer instrument on the Lunar Reconnais- Received 3 August 2015 sance Orbiter (LRO) show Tsiolkovskiy crater to have high surface rock abundance and relatively low re- Revised 6 February 2016 golith thickness.
    [Show full text]
  • Percival Lowell: the Sage As Astronomer David Sutton Dolan University of Wollongong
    University of Wollongong Research Online University of Wollongong Thesis Collection University of Wollongong Thesis Collections 1992 Percival Lowell: the sage as astronomer David Sutton Dolan University of Wollongong Recommended Citation Dolan, David Sutton, Percival Lowell: the sage as astronomer, Doctor of Philosophy thesis, Department of Science and Technology Studies, University of Wollongong, 1992. http://ro.uow.edu.au/theses/1712 Research Online is the open access institutional repository for the University of Wollongong. For further information contact the UOW Library: [email protected] PERCIVAL LOWELL: THE SAGE AS ASTRONOMER by David Sutton Dolan, B.A. Hons. (Flinders), M. A. (Adelaide) Department of Science and Techology Studies University of Wollongong January 1992 PERCIVAL LOWELL: THE SAGE AS ASTRONOMER CONTENTS CHAPTER PAGE 1. PERCIVAL LOWELL (1855-1916) IN HIS TIMES 1 1.1 Lowell's life and work 1 1.2 An overview of Lowell's astronomical writings 17 1.3 A brief survey of the biographical literature on Lowell 31 2. LOWELL IN THE LITERATURE, BEFORE THE SPACE AGE 45 2.1 C1830-1924 50 2.2 1925-49 78 2.3 1949-57 101 3. LOWELL IN THE SPACE AGE 125 3.1 Sputnik to Mariner: 1958-1965 125 3.2 Mariner to Viking and after: 1965-1990 155 4. LOWELL AND THE LITERARY PERSONA OF THE SAGE 186 4.1 Lowell as an anomaly in the pluralist tradition 188 4.2 "The eye of the man of knowledge" 204 4.3 Thomas Carlyle: Victorian prose, the universe, science and history 228 4.4 John Ruskin: the morality of landscape and climate 240 5.
    [Show full text]
  • (Aetcode) NU) BER) ______(V?
    J LUNAR DIFFERENTIAL FLUX SCANS AT 22 MICRONS (ACCFSSI0(AEtcoDE) NU) BER) ______________(V? (CAISGOY)' U(NASACR0 TMX OR A NUMBER) LUNAR DIFFERENTIAL FLUX SCANS AT 22 MICRONS Wendell W. MendelI' Space Science Departmen Rice University July, 1971 NMER)E(ACCESSIO " (T U) (NASA CR OR TMX OR AD NUM9ER) (CATEGORY) I. ABSTRACT The nighttime lunar surface has been scanned at a variety of phases both before and after new Moon. A differential chopping technique was used which records the flux difference between adjacent resolution elements along a scan. In principle the differential scan can be integrated to provide the flux distribution, but slow drifts in the sensor null level frustrated this procedure. However, some cold limb temperatures have been calculated using the planet Jupiter for calibra­ tion. The measurements were made with a resolution element of 27 arc seconds on the 28-inch telescope at the University of Arizona. Scan positions were determined by noting features on the illuminated portion of the Moon through a bore-sighted guide telescope. Positional accuracies are within two resolution elements. The technique is particularly sensitive to the detection of nighttime anomalies, and more than 150 of these have been identified. Prior to new Moon is seen large scale thermal structure, corre­ sponding to a previously unknown nonlinear cooling property of the lunar highlands. The nonlinear behavior consistently disappears 3.5 to 4 days after sunset. The effect could be due to the large scale roughness of the highlands or to a significant rock population with a mean size on the order of 10 cm.
    [Show full text]
  • Lowell Observatory Archival Material
    Lowell Observatory Archival Material August 6, 2013 In our paper, ‘Revisiting The 1963 Aristarchus Events’1, Anthony Cook and I relied heavily on documents in the Lowell Observatory Archive. We wish to thank Lowell Observatory Director Jeffrey Hall for granting us permission to post the following documents on our web site and in particular, we extend a heartfelt “Thank You” to Lowell Observatory Librarian/Archivist Lauren Amundson for her diligence in supplying us with the 305 pages of material in this document as they were being catalogued. This document contains all correspondence and related material concerning ‘The 1963 Aristarchus Events’ 2 identified in the Lowell Observatory Archives catalogued as of late 2012. This PDF file was constructed with PDF Converter Professional 7 and should also be readable with standard PDF software packages. Original scanned Lowell images were converted to PDF format and then MRC compression with text search option was applied allowing full search capabilities. For example, a PDF search of “Greenacre” should return 98 results including those on this page. This document is organized by grouping together all letters and documents sent between correspondents ordered chronologically within each grouping. For example, the first grouping of correspondence contains all letters in the Lowell Archive sent between Dr. John S. Hall and William D. Cannell starting with the earliest exchange on November 14, 1960 and continuing chronologically to the last relevant document on July 5, 1967, which was a Hall reference letter for Cannell. Some sections are simply newspaper articles or other documents placed in chronological order between correspondence groupings. There are no section headings as all documents are in a continuous flow.
    [Show full text]
  • Scientific Knowledge of the Moon, 1609 to 1969
    geosciences Review Scientific Knowledge of the Moon, 1609 to 1969 Charles A. Wood Planetary Science Institute, Tucson, AZ 85721, USA; [email protected]; Tel.: +1-301-538-5244 Received: 23 October 2018; Accepted: 18 December 2018; Published: 21 December 2018 Abstract: Discoveries stemming from the Apollo 11 mission solved many problems that had vexed scientists for hundreds of years. Research and discoveries over the preceding 360 years identified many critical questions and led to a variety of answers: How did the Moon form, how old is its surface, what is the origin of lunar craters, does the Moon have an atmosphere, how did the Moon change over time, is the Moon geologically active today, and did life play any role in lunar evolution? In general, scientists could not convincingly answer most of these questions because they had too little data and too little understanding of astronomy and geology, and were forced to rely on reasoning and speculation, in some cases wasting hundreds of years of effort. Surprisingly, by 1969, most of the questions had been correctly answered, but a paucity of data made it uncertain which answers were correct. Keywords: lunar origin; lunar crater origin; lunar atmosphere; lunar changes; lunar surface age 1. Introduction In the 360 years between Galileo’s first telescopic look at the Moon and the launch of Apollo 11, the Moon attracted many serious observers who developed questions and possible answers about its origin and conditions. Early interpretations of the Moon, its surface and atmospheric conditions were guided by philosophic beliefs from the ancient Greeks and early Christians.
    [Show full text]
  • INTERPRETATION of EXTRATERRESTRIAL IMAGERY 479 Degree Polynomial (Bowen, 1960B)
    P. M. MERIFIELD* (editor) J. M. SAARI R. 'vV. SHORTIlILL R. L. WlLDEY D. E. 'vVILHELl\'lS R. S. \VILLIAMS, JR. Interpretation of Extraterrestrial o - ) I I I ! Imagery KILOMETERS FRONTISPIECE. The multiringed basin of Mare Orientale. Lunar Orbiter IV moderate resolution photograph. Framelet width is about 90 km. Framelet orientation varies among the various Orbiter missions. (See page 489.) Note: Jorth is at the top in this and succeeding lunar photographs. (NASA photo.) Earth based telescopes; Photogeologic mapping of the Moon; Thermal mapping of the Moon; Lunar and planetary probes; Geologic interpretation of Lunar Orbiter photos; Photographic sensors for detecting extraterrestrial life. (A bslract on next page) TNTROD C'1'I0N * Chairman, Subcommittee V II, Photo Jnter­ HREE YEA RS HA VE elapsed si nce progress pretation Committee, American Society of Photo­ in the field of space imagery has been re­ grammetry, 1964-1967. Present address: Earth T Science Research Corp., Santa iVlonica, Calif. ported on to the members of the society (Van 90405. The authors are identified in their respective Lopik, Merifield, et at, 196.1), and a review of sections. 477 478 PHOTOGRAMMETRIC ENGINEERING some of the major projects that have been Ii te imagery of the earth is the subj ect of a undertaken is deemed appropriate. Terrestri­ subsequent paper to be published in this jour­ ally based telescopic photography and in­ nal. Al though this paper is intended to encolll­ frared imagery are continuing to be utilized as pass the broad spectrum of the subject, it can fundamental tools in the study of celsetial not be considered comprehensi\·e.
    [Show full text]