Appendix A. Reference List
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Lunar Impact Crater Identification and Age Estimation with Chang’E
ARTICLE https://doi.org/10.1038/s41467-020-20215-y OPEN Lunar impact crater identification and age estimation with Chang’E data by deep and transfer learning ✉ Chen Yang 1,2 , Haishi Zhao 3, Lorenzo Bruzzone4, Jon Atli Benediktsson 5, Yanchun Liang3, Bin Liu 2, ✉ ✉ Xingguo Zeng 2, Renchu Guan 3 , Chunlai Li 2 & Ziyuan Ouyang1,2 1234567890():,; Impact craters, which can be considered the lunar equivalent of fossils, are the most dominant lunar surface features and record the history of the Solar System. We address the problem of automatic crater detection and age estimation. From initially small numbers of recognized craters and dated craters, i.e., 7895 and 1411, respectively, we progressively identify new craters and estimate their ages with Chang’E data and stratigraphic information by transfer learning using deep neural networks. This results in the identification of 109,956 new craters, which is more than a dozen times greater than the initial number of recognized craters. The formation systems of 18,996 newly detected craters larger than 8 km are esti- mated. Here, a new lunar crater database for the mid- and low-latitude regions of the Moon is derived and distributed to the planetary community together with the related data analysis. 1 College of Earth Sciences, Jilin University, 130061 Changchun, China. 2 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China. 3 Key Laboratory of Symbol Computation and Knowledge Engineering of Ministry of Education, College of Computer Science and Technology, Jilin University, 130012 Changchun, China. 4 Department of Information Engineering and Computer ✉ Science, University of Trento, I-38122 Trento, Italy. -
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 -
Lecture 21: Glaciers and Paleoclimate Read: Chapter 15 Homework Due Thursday Nov
Learning Objectives (LO) Lecture 21: Glaciers and Paleoclimate Read: Chapter 15 Homework due Thursday Nov. 12 What we’ll learn today:! 1. 1. Glaciers and where they occur! 2. 2. Compare depositional and erosional features of glaciers! 3. 3. Earth-Sun orbital parameters, relevance to interglacial periods ! A glacier is a river of ice. Glaciers can range in size from: 100s of m (mountain glaciers) to 100s of km (continental ice sheets) Most glaciers are 1000s to 100,000s of years old! The Snowline is the lowest elevation of a perennial (2 yrs) snow field. Glaciers can only form above the snowline, where snow does not completely melt in the summer. Requirements: Cold temperatures Polar latitudes or high elevations Sufficient snow Flat area for snow to accumulate Permafrost is permanently frozen soil beneath a seasonal active layer that supports plant life Glaciers are made of compressed, recrystallized snow. Snow buildup in the zone of accumulation flows downhill into the zone of wastage. Glacier-Covered Areas Glacier Coverage (km2) No glaciers in Australia! 160,000 glaciers total 47 countries have glaciers 94% of Earth’s ice is in Greenland and Antarctica Mountain Glaciers are Retreating Worldwide The Antarctic Ice Sheet The Greenland Ice Sheet Glaciers flow downhill through ductile (plastic) deformation & by basal sliding. Brittle deformation near the surface makes cracks, or crevasses. Antarctic ice sheet: ductile flow extends into the ocean to form an ice shelf. Wilkins Ice shelf Breakup http://www.youtube.com/watch?v=XUltAHerfpk The Greenland Ice Sheet has fewer and smaller ice shelves. Erosional Features Unique erosional landforms remain after glaciers melt. -
The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites
Earth and Planetary Science Letters 296 (2010) 67–77 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites Mariek E. Schmidt a,⁎, Timothy J. McCoy b a Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1 b Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA article info abstract Article history: Martian basalts represent samples of the interior of the planet, and their composition reflects their source at Received 10 December 2009 the time of extraction as well as later igneous processes that affected them. To better understand the Received in revised form 16 April 2010 composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites Accepted 21 April 2010 and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from Available online 2 June 2010 K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Editor: R.W. Carlson Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is Keywords: more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior Mars igneous processes during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the shergottites residuum). -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Canyon Formation Constraints on the Discharge of Catastrophic Outburst
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Canyon formation constraints on the discharge of catastrophic 10.1002/2016JE005061 outburst floods of Earth and Mars Key Points: Mathieu G. A. Lapotre1, Michael P. Lamb1, and Rebecca M. E. Williams2 • A new model for canyon formation through waterfall retreat combines 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 2Planetary flood hydraulics and erosional mechanics Science Institute, Tucson, Arizona, USA • The model is used as a paleohydraulic tool to estimate the discharge of megafloods on Earth and Mars Abstract Catastrophic outburst floods carved amphitheater-headed canyons on Earth and Mars, and the • Compared with previous estimates, steep headwalls of these canyons suggest that some formed by upstream headwall propagation through predicted discharges are lower, fl durations higher, and water waterfall erosion processes. Because topography evolves in concert with water ow during canyon erosion, volumes are similar we suggest that bedrock canyon morphology preserves hydraulic information about canyon-forming floods. In particular, we propose that for a canyon to form with a roughly uniform width by upstream headwall retreat, erosion must occur around the canyon head, but not along the sidewalls, such that canyon width is fl fl Correspondence to: related to ood discharge. We develop a new theory for bedrock canyon formation by mega oods based M. G. A. Lapotre, on flow convergence of large outburst floods toward a horseshoe-shaped waterfall. The model is developed [email protected] for waterfall erosion by rock toppling, a candidate erosion mechanism in well fractured rock, like columnar basalt. We apply the model to 14 terrestrial (Channeled Scablands, Washington; Snake River Plain, Idaho; Citation: and Ásbyrgi canyon, Iceland) and nine Martian (near Ares Vallis and Echus Chasma) bedrock canyons and Lapotre, M. -
Washington's Channeled Scabland
t\D l'llrl,. \·· ~. r~rn1 ,uR\fEY Ut,l\n . .. ,Y:ltate" tit1Washington ALBEIT D. ROSEWNI, Governor Department of Conservation EARL COE, Dlnctor DIVISION OF MINES AND GEOLOGY MARSHALL T. HUNTTING, Supervisor Bulletin No. 45 WASHINGTON'S CHANNELED SCABLAND By J HARLEN BRETZ 9TAT• PIUHTIHO PLANT ~ OLYMPIA, WASH., 1"511 State of Washington ALBERT D. ROSELLINI, Governor Department of Conservation EARL COE, Director DIVISION OF MINES AND GEOLOGY MARSHALL T. HUNTTING, Supervisor Bulletin No. 45 WASHINGTON'S CHANNELED SCABLAND By .T HARLEN BRETZ l•or sate by Department or Conservation, Olympia, Washington. Price, 50 cents. FOREWORD Most travelers who have driven through eastern Washington have seen a geologic and scenic feature that is unique-nothing like it is to be found anywhere else in the world. This is the Channeled Scab land, a gigantic series of deeply cut channels in the erosion-resistant Columbia River basalt, the rock that covers most of the east-central and southeastern part of the state. Grand Coulee, with its spectac ular Dry Falls, is one of the most widely known features of this ex tensive set of dry channels. Many thousands of travelers must have wondered how this Chan neled Scabland came into being, and many geologists also have speculated as to its origin. Several geologists have published papers outlining their theories of the scabland's origin, but the geologist who has made the most thorough study of the problem and has ex amined the whole area and all the evidence having a bearing on the problem is Dr. J Harlen Bretz. Dr. -
Preliminary Mission Analysis and Orbit Design for Next Mars Exploration
Trans. JSASS Aerospace Tech. Japan Vol. 8, No. ists27, pp. Tk_7-Tk_12, 2010 Topics Preliminary Mission Analysis and Orbit Design for Next Mars Exploration By Naoko OGAWA 1), Mutsuko Y. MORIMOTO1), Yuichi TSUDA1,2), Tetsuya YAMADA1,2), Kazuhisa FUJITA1,3), Tomohiro YAMAGUCHI4), Yasuhiro KAWAKATSU1,2), Takashi KUBOTA1,2) and Jun’ichiro KAWAGUCHI1,2) 1)JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara, Japan 2)Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan 3)Aerospace Research and Development Directorate, Japan Aerospace Exploration Agency, Tokyo, Japan 4)The Graduate University for Advanced Studies, Sagamihara, Japan (Received July 21st, 2009) Japan has launched many interplanetary spacecraft for exploration of solar system bodies including Mars. Now we are planning the next Mars mission in the late 2010’s. This paper describes the preliminary mission analysis and orbit design for this plan. The combined exploration by several spacecraft requires complicated and careful consideration, different from those for single-probe missions. Mission plans to realize required configuration by a single launch and simple simulation results are reported. Key Words: Mars, Mission Analysis, Orbit Design, MELOS 1. Introduction 2.1.1. Meteorological orbiter for martian climate One orbiter of the two, called hereafter as the meteorological In 2008, Japan Aerospace Exploration Agency (JAXA) orbiter, aims understanding of the interaction between the has established a novel working group toward a novel Mars atmosphere and subsurface ice, and atmospheric dynamics. exploration program named MELOS, an acronym for “Mars Global, high-resolution and continuous mapping of water vapor, Exploration with Lander-Orbiter Synergy”1). As its name clouds, dusts and atmospheric temperature will be performed indicates, this is an ambitious mission composed of several with imaging cameras from the apoapsis of its highly elliptic landers and orbiters, schematically illustrated in Fig. -
The Meridiani Face on Mars
The Meridiani Face on Mars Greg Orme* School of Arts and Science, University of Queensland, Brisbane, Australia *Corresponding author: Greg Orme, School of Arts and Science, Undergraduate Science Student, University of Queensland, Brisbane, Australia, Tel: 07-33656195; E-mail: [email protected] Received: September 11, 2016; Accepted: November 25, 2016; Published: December 25, 2016 Abstract The Meridian Face has some similar features to the Cydonia and Crowned Faces such as having a crown. It is similar to the Nefertiti formation in that it seems to be made of dark soil, dunes in this case. Some dark dune fields can migrate large distances in Meridiani Planum, others remain confined in larger craters perhaps by shielding them from the wind. This can allow for the formation to be very old and remain intact. The similarity between the Crowned Face in the King’s Valley Libya Montes and the Meridiani Face was originally shown with an overall. The implicit hypothesis was that a new overlay would match the two faces even more closely, this has been borne out with the Crowned Face HiRise image and the Meridiani Face CTX image. Keywords: Meridiani planum; Barchan dune; Aeolian process; pareidolia; Dune migration Introduction The Meridiani Face was discovered around early June 2007 by a Mars researcher Terry James, (FIG. 1). The null hypothesis is that this is a random dune formation, an example of people’s innate ability to see faces [1]. It is proposed that this is falsified by the shape of these dunes, to be artificial they would have had to be moved to their current positions. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Secondary Craters on Europa and Implications for Cratered Surfaces
Vol 437|20 October 2005|doi:10.1038/nature04069 LETTERS Secondary craters on Europa and implications for cratered surfaces Edward B. Bierhaus1, Clark R. Chapman2 & William J. Merline2 For several decades, most planetary researchers have regarded the craters were typically not spatially random, but instead appeared in impact crater populations on solid-surfaced planets and smaller clumps and clusters16 even at distances far (several hundred kilo- bodies as predominantly reflecting the direct (‘primary’) impacts metres) from the nearest large primary crater. This clustered spatial of asteroids and comets1. Estimates of the relative and absolute distribution contrasts with primary impacts, which are spatially ages of geological units on these objects have been based on this random. The low spatial density and unusual non-random spatial assumption2. Here we present an analysis of the comparatively distribution of Europa’s small craters enabled us to achieve what has sparse crater population on Jupiter’s icy moon Europa and suggest been previously difficult, namely unambiguous identification and that this assumption is incorrect for small craters. We find that quantification of the contribution of distant secondary craters to the ‘secondaries’ (craters formed by material ejected from large total crater SFD. This, in turn, allows us to re-examine the overall primary impact craters) comprise about 95 per cent of the small crater age-dating methodology. We discuss the specifics of the craters (diameters less than 1 km) on Europa. We therefore con- Europa data first. clude that large primary impacts into a solid surface (for example, We measured more than 17,000 craters in 87 low-compression, ice or rock) produce far more secondaries than previously low-sun, high-resolution Europa images (scales ,60 m pixel21), believed, implying that the small crater populations on the which cover nine regions totalling 0.2% of Europa’s surface (a much Moon, Mars and other large bodies must be dominated by larger percentage of Europa has been imaged at lower resolutions), secondaries. -
WILKINSON COLLEGE of Arts, Humanities, and Social Sciences
2014 – 2015 WILKINSON COLLEGE of Arts, Humanities, and Social Sciences ANNUAL REPORT 2 Table of Contents Opening Statement ..........................................................................................................................................2-3 International Reach ........................................................................................................................................ 4-5 CRASsH and BURN .......................................................................................................................................6-7 Collections in Wilkinson ..................................................................................................................................8 Creative Industries .............................................................................................................................................9 Arts and Humanities................ ...................................................................................................................10-25 Art ....................................................................................................................................................10-11 English .............................................................................................................................................12-13 World Languages & Cultures .......................................................................................................14-15 Religious Studies ............................................................................................................................16-17