CNN-Based High-Resolution 3D Reconstruction of the Martian Surface from Single Images
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Wind Measurements of Martian Dust Devils from Hirise
EPSC Abstracts Vol. 6, EPSC-DPS2011-570, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Wind Measurements of Martian Dust Devils from HiRISE D. S. Choi (1) and C. M. Dundas (2) (1) Department of Planetary Sciences, University of Arizona, Tucson, AZ, USA ([email protected]) (2) United States Geological Survey, Flagstaff, AZ, USA Abstract servation crosses an active feature such as a dust devil, changes in the active feature are apparent from the We report direct measurements of the winds within three separate views. Treating the dust clouds as pas- Martian dust devils from HiRISE imagery. The cen- sive tracers of motion then allows for the direct mea- tral color swath of the HiRISE instrument observes surement of wind velocities. the surface by using separate CCDs and color filters in We utilize measurements from manual (hand-eye) rapid cadence. Active features, such as a dust devil, tracking of the clouds through image blinking, as appear in motion when serendipitously captured by well as automated correlation methods [9]. Typically, this region of the instrument. Our measurements re- manual measurements are more successful than au- veal clear circulation within the vortices, and that the tomated measurements. The relatively diffuse dust majority of overall wind magnitude within a dust devil clouds, combined with the static background terrain, 1 is between 10 and 30 m s− . cause the automated software to incorrectly report the movement as stationary. Successful automated results were obtained from images with more substantial dust 1. Introduction clouds and relatively featureless background terrain. Direct measurements of the winds within a Martian dust devil [1] are challenging to obtain. -
Mars Reconnaissance Orbiter
Chapter 6 Mars Reconnaissance Orbiter Jim Taylor, Dennis K. Lee, and Shervin Shambayati 6.1 Mission Overview The Mars Reconnaissance Orbiter (MRO) [1, 2] has a suite of instruments making observations at Mars, and it provides data-relay services for Mars landers and rovers. MRO was launched on August 12, 2005. The orbiter successfully went into orbit around Mars on March 10, 2006 and began reducing its orbit altitude and circularizing the orbit in preparation for the science mission. The orbit changing was accomplished through a process called aerobraking, in preparation for the “science mission” starting in November 2006, followed by the “relay mission” starting in November 2008. MRO participated in the Mars Science Laboratory touchdown and surface mission that began in August 2012 (Chapter 7). MRO communications has operated in three different frequency bands: 1) Most telecom in both directions has been with the Deep Space Network (DSN) at X-band (~8 GHz), and this band will continue to provide operational commanding, telemetry transmission, and radiometric tracking. 2) During cruise, the functional characteristics of a separate Ka-band (~32 GHz) downlink system were verified in preparation for an operational demonstration during orbit operations. After a Ka-band hardware anomaly in cruise, the project has elected not to initiate the originally planned operational demonstration (with yet-to-be used redundant Ka-band hardware). 201 202 Chapter 6 3) A new-generation ultra-high frequency (UHF) (~400 MHz) system was verified with the Mars Exploration Rovers in preparation for the successful relay communications with the Phoenix lander in 2008 and the later Mars Science Laboratory relay operations. -
The Analysis of Life Struggle in Andy Weir's
THE ANALYSIS OF LIFE STRUGGLE IN ANDY WEIR‘S NOVEL THE MARTIAN A THESIS BY ALEMINA BR KABAN REG. NO. 140721012 DEPARTMENT OF ENGLISH FACULTY OF CULTURAL STUDIES UNIVERSITY OF SUMATERA UTARA MEDAN 2018 UNIVERSITAS SUMATERA UTARA THE ANALYSIS OF LIFE STRUGGLE IN ANDY WEIR‘S NOVEL THE MARTIAN A THESIS BY ALEMINA BR KABAN REG. NO. 140721012 SUPERVISOR CO-SUPERVISOR Drs. Parlindungan Purba,M.Hum. Riko Andika Pohan, S.S., M.Hum. NIP.1963021619 89031003001 NIP. 1984060920150410010016026 Submitted to Faculty of Cultural Studies University of Sumatera Utara Medan in partial fulfilment of the requirements for the degree of Sarjana Sastra from Department of English DEPARTMENT OF ENGLISH FACULTY OF CULTURAL STUDIES UNIVERSITY OF SUMATERA UTARA MEDAN 2018 UNIVERSITAS SUMATERA UTARA Approved by the Department of English, Faculty of Cultural Studies University of Sumatera Utara (USU) Medan as thesis for The Sarjana Sastra Examination. Head, Secretary, Prof. T.Silvana Sinar,Dipl.TEFL,MA.,Ph.D Rahmadsyah Rangkuti, M.A. Ph.D. NIP. 19571117 198303 2 002 NIP. 19750209 200812 1 002 UNIVERSITAS SUMATERA UTARA Accepted by the Board of Examiners in partial fulfillment of requirements for the degree of Sarjana Sastra from the Department of English, Faculty of Cultural Studies University of Sumatera Utara, Medan. The examination is held in Department of English Faculty of Cultural Studies University of Sumatera Utara on July 6th, 2018 Dean of Faculty of Cultural Studies University of Sumatera Utara Dr. Budi Agustono, M.S. NIP.19600805 198703 1 001 Board of Examiners Rahmadsyah Rangkuti, M.A., Ph.D __________________ Drs. Parlindungan Purba, M.Hum. -
Lafayette - 800 Grams Nakhlite
Lafayette - 800 grams Nakhlite Figure 1. Photograph showing fine ablation features Figure 2. Photograph of bottom surface of Lafayette of fusion crust on Lafayette meteorite. Sample is meteorite. Photograph from Field Museum Natural shaped like a truncated cone. This is a view of the top History, Chicago, number 62918. of the cone. Sample is 4-5 centimeters across. Photo- graph from Field Museum Natural History, Chicago, number 62913. Introduction According to Graham et al. (1985), “a mass of about 800 grams was noticed by Farrington in 1931 in the geological collections in Purdue University in Lafayette Indiana.” It was first described by Nininger (1935) and Mason (1962). Lafayette is very similar to the Nakhla and Governador Valadares meteorites, but apparently distinct from them (Berkley et al. 1980). Lafayette is a single stone with a fusion crust showing Figure 3. Side view of Lafayette. Photograph from well-developed flow features from ablation in the Field Museum Natural History, Chicago, number Earth’s atmosphere (figures 1,2,3). The specimen is 62917. shaped like a rounded cone with a blunt bottom end. It was apparently oriented during entry into the Earth’s that the water released during stepwise heating of atmosphere. Note that the fine ablation features seen Lafayette was enriched in deuterium. The alteration on Lafayette have not been reported on any of the assemblages in Lafayette continue to be an active field Nakhla specimens. of research, because it has been shown that the alteration in Lafayette occurred on Mars. Karlsson et al. (1992) found that Lafayette contained the most extra-terrestrial water of any Martian Lafayette is 1.32 b.y. -
An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger Depauw University
DePauw University Scholarly and Creative Work from DePauw University Student research Student Work 2015 An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger DePauw University Follow this and additional works at: http://scholarship.depauw.edu/studentresearch Part of the Economics Commons, and the The unS and the Solar System Commons Recommended Citation Knappenberger, Clayton, "An Economic Analysis of Mars Exploration and Colonization" (2015). Student research. Paper 28. This Thesis is brought to you for free and open access by the Student Work at Scholarly and Creative Work from DePauw University. It has been accepted for inclusion in Student research by an authorized administrator of Scholarly and Creative Work from DePauw University. For more information, please contact [email protected]. An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger 2015 Sponsored by: Dr. Villinski Committee: Dr. Barreto and Dr. Brown Contents I. Why colonize Mars? ............................................................................................................................ 2 II. Can We Colonize Mars? .................................................................................................................... 11 III. What would it look like? ............................................................................................................... 16 A. National Program ......................................................................................................................... -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Mro High Resolution Imaging Science Experiment (Hirise)
Sixth International Conference on Mars (2003) 3287.pdf MROHIGHRESOLUTIONIMAGINGSCIENCEEXPERIMENT(HIRISE): INSTRUMENTDEVELOPMENT.AlanDelamere,IraBecker,JimBergstrom,JonBurkepile,Joe Day,DavidDorn,DennisGallagher,CharlieHamp,JeffreyLasco,BillMeiers,AndrewSievers,Scott StreetmanStevenTarr,MarkTommeraasen,PaulVolmer.BallAerospaceandTechnologyCorp.,PO Box1062,Boulder,CO80306 Focus Introduction:Theprimaryfunctionalre- Mechanism PrimaryMirror quirementoftheHiRISEimager,figure1isto PrimaryMirrorBaffle 2nd Fold allowidentificationofbothpredictedandun- Mirror knownfeaturesonthesurfaceofMarstoa muchfinerresolutionandcontrastthanprevi- ouslypossible[1],[2].Thisresultsinacam- 1st Fold erawithaverywideswathwidth,6kmat Mirror 300kmaltitude,andahighsignaltonoise ratio,>100:1.Generationofterrainmaps,30 Filters cmverticalresolution,fromstereoimages Focal requiresveryaccurategeometriccalibration. Plane Theprojectlimitationsofmass,costand schedulemakethedevelopmentchallenging. FocalPlane SecondaryMirror Inaddition,thespacecraftstability[3]must Electronics TertiaryMirror SecondaryMirrorBaffle notbeamajorlimitationtoimagequality. Thenominalorbitforthesciencephaseofthe missionisa3pmorbitof255by320kmwith Figure1Cameraopticalpathoptimizedforlowmass periapsislockedtothesouthpole.Thetrack Integration(TDI)tocreateveryhigh(100:1)signalnoise velocityisapproximately3,400m/s. ratioimages. HiRISEFeatures:TheHiRISEinstrumentperformance Theimagerdesignisanall-reflectivethreemirrorastig- goalsarelistedinTable1.Thedesignfeaturesa50cm matictelescopewithlight-weightedZeroduropticsanda -
Secondary Minerals in the Nakhlite Meteorite Yamato 000593: Distinguishing Martian from Terrestrial Alteration Products
46th Lunar and Planetary Science Conference (2015) 2010.pdf SECONDARY MINERALS IN THE NAKHLITE METEORITE YAMATO 000593: DISTINGUISHING MARTIAN FROM TERRESTRIAL ALTERATION PRODUCTS. H. Breton1, M. R. Lee1, and D. F. Mark2 1School of Geographical and Earth Sciences, University of Glasgow, University Ave, Glasgow, Lanarkshire G12 8QQ, UK ([email protected]), 2Scottish Universities Environmental Research Center, Rankine Ave, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK Introduction: The nakhlites are olivine-bearing Methods: A thin section of Y-000593 was studied clinopyroxenites that formed in a Martian lava flow or using a Carl Zeiss Sigma field-emission SEM equipped shallow intrusion 1.3 Ga ago [1, 2]. They are scientifi- with an Oxford Instruments Aztec microanalysis sys- cally extremely valuable because they interacted with tem at the University of Glasgow. Chemical and miner- water-bearing fluids on Mars [3]. Fluid-rock interac- alogical identification within the secondary minerals tions led to the precipitation of secondary minerals, were obtained through backscattered electron (BSE) many of which are hydrous. The secondary minerals imaging and energy dispersive spectroscopy (EDS) consist in a mixture of poorly crystalline smectitic ma- mapping and quantitative microanalysis. terial and Fe-oxide, collectively called “iddingsite”, but Results and discussions: Y-000593 is an unbrec- also carbonate and sulphate [4]. The proportion, chem- ciated cumulate rock whose mineralogy is similar to istry and habit of the secondary minerals vary between other nakhlites: a predominance of augite and minor members of the Nakhlite group, which is thought to olivine phenocrysts surrounded by a microcrystalline reflect compositional variation of the fluid within the mesostasis [9]. -
Optimal Reconfiguration Maneuvers for Spacecraft
58th International Astronautical Congress, Hyderabad, 24-28 September 2007. Copyright 2007 by Lindsay Millard. Published by the IAF, with permission and Released to IAF or IAA to publish in all forms. IACIAC----07070707----C1.7.03C1.7.03 OOOPTPTPTIMALPT IMAL RRRECONFIGURATION MMMANEUVERS FFFORFOR SSSPACECRAFT IIIMAGING AAARRAYS IN MMMULTI ---B-BBBODY RRREGIMES Lindsay D. Millard Graduate Student School of Aeronautics and Astronautics Purdue University West Lafayette, Indiana [email protected] Kathleen C. Howell Hsu Lo Professor of Aeronautical and Astronautical Engineering School of Aeronautics and Astronautics Purdue University West Lafayette, Indiana [email protected] AAABSTRACT Upcoming National Aeronautics and Space Administration (NASA) mission concepts include satellite arrays to facilitate imaging and identification of distant planets. These mission scenarios are diverse, including designs such as the Terrestrial Planet Finder-Occulter (TPF-O), where a monolithic telescope is aided by a single occulter spacecraft, and the Micro-Arcsecond X-ray Imaging Mission (MAXIM), where as many as sixteen spacecraft move together to form a space interferometer. Each design, however, requires precise reconfiguration and star-tracking in potentially complex dynamic regimes. This paper explores control methods for satellite imaging array reconfiguration in multi-body systems. Specifically, optimal nonlinear control and geometric control methods are derived and compared to the more traditional linear quadratic regulators, as well as to input state feedback linearization. These control strategies are implemented and evaluated for the TPF-O mission concept. IIINTRODUCTION Over the next two decades, one focus of NASA‘s Upcoming National Aeronautics and Space Origins program is the development of sophisticated Administration (NASA) mission concepts include telescopes and technologies to begin a search for satellite formations to facilitate imaging and extraterrestrial life and to monitor the birth of identification of distant planets. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
An Implementation Concept for the ASPIRE Mission
An Implementation Concept for the ASPIRE Mission. W. D. Deininger* ([email protected]), W. Purcell,* P. Atcheson,*G. Mills,* S. A Sandford,** R. P. Hanel,** M. McKelvey,** and R. McMurray** *Ball Aerospace & Technologies Corp. (BATC) P. O. Box 1062 Boulder, CO, USA 80306-1062 **NASA Ames Research Center Moffett Field, CA, USA 94035 Abstract—The Astrobiology Space Infrared Explorer complex and tied to the cyclic process whereby these (ASPIRE) is a Probe-class mission concept developed as elements are ejected into the diffuse interstellar medium part of NASA’s Astrophysics Strategic Mission Concept (ISM) by dying stars, gathered into dense clouds and studies. 1 2 ASPIRE uses infrared spectroscopy to explore formed into the next generation of stars and planetary the identity, abundance, and distribution of molecules, systems (Figure 1). Each stage in this cycle entails chemical particularly those of astrobiological importance throughout alteration of gas- and solid-state species by a diverse set of the Universe. ASPIRE’s observational program is focused astrophysical processes: hocks, stellar winds, radiation on investigating the evolution of ices and organics in all processing by photons and particles, gas-phase neutral and phases of the lifecycle of carbon in the universe, from ion chemistry, accretion, and grain surface reactions. These stellar birth through stellar death while also addressing the processes create new species, destroy old ones, cause role of silicates and gas-phase materials in interstellar isotopic enrichments, shuffle elements between chemical organic chemistry. ASPIRE achieves these goals using a compounds, and drive the universe to greater molecular Spitzer-derived, cryogenically-cooled, 1-m-class telescope complexity.