13. Martian Cratering and Implications for the Chronostratigraphy
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Planetary Geologic Mappers Annual Meeting
Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m. -
Curiosity's Candidate Field Site in Gale Crater, Mars
Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell -
Copyrighted Material
Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
Supervolcanoes Within an Ancient Volcanic Province in Arabia Terra, Mars 2 3 4 Joseph
EMBARGOED BY NATURE 1 1 Supervolcanoes within an ancient volcanic province in Arabia Terra, Mars 2 3 4 Joseph. R. Michalski 1,2 5 1Planetary Science Institute, Tucson, Arizona 85719, [email protected] 6 2Dept. of Earth Sciences, Natural History Museum, London, United Kingdom 7 8 Jacob E. Bleacher3 9 3NASA Goddard Space Flight Center, Greenbelt, MD, USA. 10 11 12 Summary: 13 14 Several irregularly shaped craters located within Arabia Terra, Mars represent a 15 new type of highland volcanic construct and together constitute a previously 16 unrecognized martian igneous province. Similar to terrestrial supervolcanoes, these 17 low-relief paterae display a range of geomorphic features related to structural 18 collapse, effusive volcanism, and explosive eruptions. Extruded lavas contributed to 19 the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulfur 20 and erupted fine-grained pyroclastics from these calderas likely fed the formation of 21 altered, layered sedimentary rocks and fretted terrain found throughout the 22 equatorial region. Discovery of a new type of volcanic construct in the Arabia 23 volcanic province fundamentally changes the picture of ancient volcanism and 24 climate evolution on Mars. Other eroded topographic basins in the ancient Martian 25 highlands that have been dismissed as degraded impact craters should be 26 reconsidered as possible volcanic constructs formed in an early phase of 27 widespread, disseminated magmatism on Mars. 28 29 30 EMBARGOED BY NATURE 2 31 The source of fine-grained, layered deposits1,2 detected throughout the equatorial 32 region of Mars3 remains unresolved, though the deposits are clearly linked to global 33 sedimentary processes, climate change, and habitability of the surface4. -
Annual Report COOPERATIVE INSTITUTE for RESEARCH in ENVIRONMENTAL SCIENCES
2015 Annual Report COOPERATIVE INSTITUTE FOR RESEARCH IN ENVIRONMENTAL SCIENCES COOPERATIVE INSTITUTE FOR RESEARCH IN ENVIRONMENTAL SCIENCES 2015 annual report University of Colorado Boulder UCB 216 Boulder, CO 80309-0216 COOPERATIVE INSTITUTE FOR RESEARCH IN ENVIRONMENTAL SCIENCES University of Colorado Boulder 216 UCB Boulder, CO 80309-0216 303-492-1143 [email protected] http://cires.colorado.edu CIRES Director Waleed Abdalati Annual Report Staff Katy Human, Director of Communications, Editor Susan Lynds and Karin Vergoth, Editing Robin L. Strelow, Designer Agreement No. NA12OAR4320137 Cover photo: Mt. Cook in the Southern Alps, West Coast of New Zealand’s South Island Birgit Hassler, CIRES/NOAA table of contents Executive summary & research highlights 2 project reports 82 From the Director 2 Air Quality in a Changing Climate 83 CIRES: Science in Service to Society 3 Climate Forcing, Feedbacks, and Analysis 86 This is CIRES 6 Earth System Dynamics, Variability, and Change 94 Organization 7 Management and Exploitation of Geophysical Data 105 Council of Fellows 8 Regional Sciences and Applications 115 Governance 9 Scientific Outreach and Education 117 Finance 10 Space Weather Understanding and Prediction 120 Active NOAA Awards 11 Stratospheric Processes and Trends 124 Systems and Prediction Models Development 129 People & Programs 14 CIRES Starts with People 14 Appendices 136 Fellows 15 Table of Contents 136 CIRES Centers 50 Publications by the Numbers 136 Center for Limnology 50 Publications 137 Center for Science and Technology -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
Technical Note
NASA TN D-1493 O5 C,/ 1-4 I Q LOAJN' ? < TECHNICAL NOTE D-1493 ENVIRONMENTAL PROBLEMS OF SPACE FLIGHT STRUCTURES H. METEOROID HAZARD Prepared by John R. Davidson and Paul E. Sandorff in collaboration with the NASA Research Advisory Committee on Missile and Space Vehicle Structures Langley Research Center Langley Station, Hampton, Va. NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON January 1963 TECH LIBRARY KAFB, NM Illllllll TABLE OF CONTENTS 0153^57 Page PREFACE li MEMBERS OF THE NASA RESEARCH ADVISORY COMMITTEE ON MISSILE AND SPACE VEHICLE STRUCTURES in SUMMARY 1 INTRODUCTION 1 SYMBOLS -. 2 METEOROID ENVIRONMENT ^ Asteroidal Particles ; . k Cometary Particles 5 Tektites 8 Pertubation Forces 9 Observations of Meteors From the Earth 10 Satellites and Space Probes 15 Research in Progress 18 INTERACTION BETWEEN METEOROID ENVIRONMENT AND STRUCTURE 19 Historical Aspects of the Plate Perforation Problem 19 Physical Description of High-Speed Impact Phenomena 20 Modern Theories of Penetration 22 Experimental Data .__ 26 PROTECTION METHODS 30 Types of Structural Damage 30 Application of Meteoroid Flux Data and Impact Data to Design Problems 30 RESEARCH IN PROGRESS 36 Ground Research 36 Flight Test Research 36 RECOMMENDED METEOROID RESEARCH PROGRAM 36 REFERENCES kO BIBLIOGRAPHY 1*7 TABLES 49 FIGURES 61 PREFACE The exploration, study, and definition of the environmental conditions which exist in space beyond the earth's atmosphere form an essential part of the current space-age effort. The development of this science is of especial interest to the vehicle structures designer, who must make decisions today that will establish the capability and efficiency of the space hardware in use 5 °r 10 years hence. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
Worry Over Mistreating Clots Drove Push to Pause J&J Shot
P2JW109000-6-A00100-17FFFF5178F ****** MONDAY,APRIL 19,2021~VOL. CCLXXVII NO.90 WSJ.com HHHH $4.00 Last week: DJIA 34200.67 À 400.07 1.2% NASDAQ 14052.34 À 1.1% STOXX 600 442.49 À 1.2% 10-YR. TREASURY À 27/32 , yield 1.571% OIL $63.13 À $3.81 EURO $1.1982 YEN 108.81 Bull Run What’s News In Stocks Widens, Business&Finance Signaling More stocks have been propelling the U.S. market higher lately,asignal that fur- Strength ther gains could be ahead, but howsmooth the climb might be remains up fordebate. A1 Technical indicators WeWork’s plan to list suggestmoregains, stock by merging with a but some question how blank-check company has echoes of its approach in smooth theywill be 2019,when the shared-office provider’s IPO imploded. A1 BY CAITLIN MCCABE Citigroup plans to scale up its services to wealthy GES Agreater number of stocks entrepreneurs and their IMA have been propelling the U.S. businesses in Asia as the market higher lately,asignal bank refocuses its opera- GETTY that—if historyisany indica- tions in the region. B1 SE/ tor—moregains could be ahead. What remains up forde- A Maryland hotel mag- bate, however, is how smooth natebehind an 11th-hour bid ANCE-PRES FR the climb will be. to acquireTribune Publish- Indicatorsthat point to a ing is working to find new ENCE stronger and moreresilient financing and partnership AG stock market have been hitting options after his partner ON/ LL rare milestones recently as the withdrew from the deal. -
Thickness of the Martian Crust: Improved Constraints from Geoid-To-Topography Ratios Mark A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109, E01009, doi:10.1029/2003JE002153, 2004 Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios Mark A. Wieczorek De´partement de Ge´ophysique Spatiale et Plane´taire, Institut de Physique du Globe de Paris, Saint-Maur, France Maria T. Zuber Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA Received 10 July 2003; revised 1 September 2003; accepted 24 November 2003; published 24 January 2004. [1] The average crustal thickness of the southern highlands of Mars was investigated by calculating geoid-to-topography ratios (GTRs) and interpreting these in terms of an Airy compensation model appropriate for a spherical planet. We show that (1) if GTRs were interpreted in terms of a Cartesian model, the recovered crustal thickness would be underestimated by a few tens of kilometers, and (2) the global geoid and topography signals associated with the loading and flexure of the Tharsis province must be removed before undertaking such a spatial analysis. Assuming a conservative range of crustal densities (2700–3100 kg mÀ3), we constrain the average thickness of the Martian crust to lie between 33 and 81 km (or 57 ± 24 km). When combined with complementary estimates based on crustal thickness modeling, gravity/topography admittance modeling, viscous relaxation considerations, and geochemical mass balance modeling, we find that a crustal thickness between 38 and 62 km (or 50 ± 12 km) is consistent with all studies. Isotopic investigations based on Hf-W and Sm-Nd systematics suggest that Mars underwent a major silicate differentiation event early in its evolution (within the first 30 Ma) that gave rise to an ‘‘enriched’’ crust that has since remained isotopically isolated from the ‘‘depleted’’ mantle. -
Workshop on the Martiannorthern Plains: Sedimentological,Periglacial, and Paleoclimaticevolution
NASA-CR-194831 19940015909 WORKSHOP ON THE MARTIANNORTHERN PLAINS: SEDIMENTOLOGICAL,PERIGLACIAL, AND PALEOCLIMATICEVOLUTION MSATT ..V",,2' :o_ MarsSurfaceandAtmosphereThroughTime Lunar and PlanetaryInstitute 3600 Bay AreaBoulevard Houston TX 77058-1113 ' _ LPI/TR--93-04Technical, Part 1 Report Number 93-04, Part 1 L • DISPLAY06/6/2 94N20382"£ ISSUE5 PAGE2088 CATEGORY91 RPT£:NASA-CR-194831NAS 1.26:194831LPI-TR-93-O4-PT-ICNT£:NASW-4574 93/00/00 29 PAGES UNCLASSIFIEDDOCUMENT UTTL:Workshopon the MartianNorthernPlains:Sedimentological,Periglacial, and PaleoclimaticEvolution TLSP:AbstractsOnly AUTH:A/KARGEL,JEFFREYS.; B/MOORE,JEFFREY; C/PARKER,TIMOTHY PAA: A/(GeologicalSurvey,Flagstaff,AZ.); B/(NationalAeronauticsand Space Administration.GoddardSpaceFlightCenter,Greenbelt,MD.); C/(Jet PropulsionLab.,CaliforniaInst.of Tech.,Pasadena.) PAT:A/ed.; B/ed.; C/ed. CORP:Lunarand PlanetaryInst.,Houston,TX. SAP: Avail:CASIHC A03/MFAOI CIO: UNITEDSTATES Workshopheld in Fairbanks,AK, 12-14Aug.1993;sponsored by MSATTStudyGroupandAlaskaUniv. MAJS:/*GLACIERS/_MARSSURFACE/*PLAINS/*PLANETARYGEOLOGY/*SEDIMENTS MINS:/ HYDROLOGICALCYCLE/ICE/MARS CRATERS/MORPHOLOGY/STRATIGRAPHY ANN: Papersthathavebeen acceptedforpresentationat the Workshopon the MartianNorthernPlains:Sedimentological,Periglacial,and Paleoclimatic Evolution,on 12-14Aug. 1993in Fairbanks,Alaskaare included.Topics coveredinclude:hydrologicalconsequencesof pondedwateron Mars; morpho!ogical and morphometric studies of impact cratersin the Northern Plainsof Mars; a wet-geology and cold-climateMarsmodel:punctuation