DOCSLIB.ORG

Mariner 9 View of Mars' Surface Taken from 5400 Km Range

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Mariner 9 View of Mars' Surface Taken from 5400 Km Range FIG.1. Mariner 9 view of Mars' surface taken from 5400 km range. A few control points are marked and the pixel counting grid can be seen. MERTONE. DAVIES Rand Corporation Santa Monica, Calif. 90406 Mariner 9: Primary Control Net The control net of Mars is being computed photogrammetrically from the television pictures taken by the spacecraft during its active year in orbit around Mars. (Abstract on next page) indeed to the planet Earth. WEARE in the midst of what is perhaps Cartography is the language of explora- man's greatest exploration-the explora- tion; it has proved to be the most useful way tion of the major bodies of the solar system. to visualize a region, to locate landmarks This great adventure is a consequence of the within it, and to estimate distances and di- conscious efforts of men with vision to ex- rections. The coordinate system of the map ploit the ingenuity of modem engineering to is the basis for navigation, for describing and seek out and examine distant worlds. This communicating specific locations, and for ancient dream of exploration started soon finding known landmarks. From an historical after the beginning of the space age and now point of view, maps of a region produced at initial contacts have been made with the different periods reflect changes to the region Moon, Venus, and Mars; Mercury will soon with time and also portray the rate of in- be added and then the excitingly distant creased knowledge of the details of the area. outer planetary systems. Like the important Improvement in the positional data of land- explorations of the past, it is difficult to per- marks can be observed as more refined meas- ceive adequately the value of those hitherto urements are introduced into the determina- unknown worlds to future generations, and tion of coordinates. Unmanned missions are of different types the wide-angle lens (the 50-mm focal length -some are flybys, some are orbiters, and lens). The vidicon format was 9.8 mm x some are landers; they carry scientific instru- 12.5 mm, giving a field of view of 11" x 14", ments that are appropriate to the particular a much narrower field of view than is usual mission. A group of experimenters are ap- on mapping cameras. The television readout pointed to the mission to participate in the sampled each line 832 times and scanned design, calibration, and use of each instru- 700 lines per frame. The characteristics of ment to assure the maximum return of use- the wide-angle television camera are sum- ful data. As a member of the television ex- marized in Table 1; also listed are the size perimenter team, I should like to describe of an individual sample or pixel (picturc how a new primary control net of Mars is element) and the footprint measured on the being computed photogrammetrically from object surface with the camera located vari- the pictures taken by the Mariner 9 space- ous distances normal to this plane surface. craft during its active year in orbit around The vidicon camera is a relatively poor in- Mars. First is a discussion of the pictures, strument for making photogrammetric reduc- their characteristics, and distribution, then tions because the format is small and the an examination of the control points, and electronic distortions are large. Difficulties finally, a review of the computation of the in removingu these distortions lead to standard control net and its status. errors of frame measurements of at least 15 ABSTRACT:A planetwide control net of Mars is being derived photo- grammetrically from the television pictures that were returned by Mariner 9. Such a control net is required by cartographers to relate the coordinate system to landmarks and topography. Although the pictures cover the entire Mars surface, there are gaps in the low- resolution coverage. The vidicon camera, which produced the photos used in the control net computations, is a poor instrument for photo- grammetric analysis because the electronic distortions are large and the format is small. The coordinate system incorporates a new direction for the spin axis of Mars, a prime meridian defined by a particular crater (Airy-0) on the surface, and a particular reference spheroid for aero- graphic coordinates. The computation of the primary control net is a continuing project; as of June 1973 it contained 1645 control points. THE PICTURES pm. A useful index of the value of a camera The Mariner 9 spacecraft contained two system for photogrammetric computations is television cameras-one with a 50-mm focal- found by dividing the format dimensions by length lens and the other with a 500-mm the measurement errors. For this vidicon, focal-length lens. All of the pictures used in 9.6/0.015 = 6.4 x 102, 12.5/0.015 = 8.3 the control net computations were taken with x 102. A few years ago Duane Brown (1968) reported on a study of a hypothetical lunar control network. This elegant study demon- strated the power of the photogrammetric Sensor-slow scan vidicon solution of the closed control net to deter- Optics-Zeiss Planar, 50-mm focal length, f/2 mine the geometric shape of a planetary stopped down to f/4 body. Brown assumed that a dedicated Format-9.6 mm x 12.5 mm, 700 x 832 pixels spacecraft was placed in optimum orbit for Field of view-11 " x 14" this mission and that it was instrumented with a 9-in. x 9-in. format photographic film Normal Distance to Plane Surface Pixel Size Footprint camera. The standard error of the measure- (km) (km) (km) ments was assumed to be 3 pm, so that the photogrammetric index was 225/0.003 = 7.5 0.56 380 x 500 x 104. The hypothetical camera is thus two 0.84 580 750 orders of magnitude better than the Mariner 1.1 770 1000 9 vidicon for this type of solution. In addi- 1.4 960 X 1250 1.7 1150 1500 tion, the Mariner 9 orbit was far from optimum. Although it is clear that the ac- MARINER 9: PRIMARY CONTROL NET curacy of the results from Mariner 9 will not region as Fig. 1, thus forming a tie between approach that of Brown's study, his study the sequences. The control points that were was valuable in planning this phase of the measured on these frames have been circled. Mariner 9 experiment. It is also useful in The measurements are made by counting suggesting methods for obtaining improved pixels on frames like these, which have had results on future missions. no geometric processing; the frames have The Mariner 9 spacecraft was in a 12-hour been high-pass filtered and stretched to bring orbit with a 65" inclination; periapsis altitude out details, and a special grid is introduced was 1600 km, initially located at about 2F0 that accentuates every 25 and 100 pixels to south latitude. Highest priority was assigned aid in counting. to mapping sequences designed to obtain In the northern hemisphere, geodesy se- continuous pictures of the entire surface of quences acquired pictures (from a distance the planet at maximum resolution with the of about 3000 km) of the region between 50-mm focal length lens camera. The map- the equator and 30" north. North of these ping frames taken near periapsis have too to the pole, mapping frames taken from dis- small coverage to be useful in the computa- tances of 3000 to 4500 km are used in the tions of the control net. The geodesy se- control net computations. quences contained frames taken from 3000 to The most serious coverage gap exists in 6000 km altitude with considerable overlan.A, the south between latitude -30" and the and were designed for the computation of equator, where the only useful frames are the the planetwide control net. Unfortunately, mapping pictures. These frames have very full coverage of the planet was not obtained little overlap and were taken near periapsis with these pictures, so it is necessary to fill at altitudes of less than 2000 km. At this some gaps in coverage using mapping frames. distance, many hundreds of frames are re- Figure 1 was taken from a distance of quired to obtain full surface coverage. The about 5400 km and is typical of these very primary control net thus contains a few bands useful frames. Pictures from this distance across this region to tie the northern and cover the southern hemisphere from latitude southern hemispheres together. -30" to -70" except for gaps in longitude Most of the control points are the centers at 90" and 270". The south polar region was of craters a few kilometers in diameter. Meas- covered by frames taken from distances of urements, with an origin at the upper left 3000 to 3500 km. Figure 2 is an example hand corner, are made by counting pixels on of one frame that was taken of the same pictures that have had no geometric process- FIG.2. Mariner 9 view of Mars' sur taken f~ 3200 lun range. A few control points are marked and the pixel counting grid can be seen. ing. Using the reseau point locations and a of 1950.0 current use in the American program developed by John Kreznar (1973) Ephemeris is a, = 316."85, 8, = 53."01. to remove the geometric distortions, the pixel The corresponding values for the Mariner 9 measurements are converted to coordinates coordinate system are a, = 317."32, 8, = in the focal plane with the origin at the 52. " 68. principal point. The exact focal length of the The prime meridian is defined in the lens is 52.267 mm.
Load more

Recommended publications
  • Railway Employee Records for Colorado Volume Iii
    RAILWAY EMPLOYEE RECORDS FOR COLORADO VOLUME III By Gerald E. Sherard (2005) When Denver’s Union Station opened in 1881, it saw 88 trains a day during its gold-rush peak. When passenger trains were a popular way to travel, Union Station regularly saw sixty to eighty daily arrivals and departures and as many as a million passengers a year. Many freight trains also passed through the area. In the early 1900s, there were 2.25 million railroad workers in America. After World War II the popularity and frequency of train travel began to wane. The first railroad line to be completed in Colorado was in 1871 and was the Denver and Rio Grande Railroad line between Denver and Colorado Springs. A question we often hear is: “My father used to work for the railroad. How can I get information on Him?” Most railroad historical societies have no records on employees. Most employment records are owned today by the surviving railroad companies and the Railroad Retirement Board. For example, most such records for the Union Pacific Railroad are in storage in Hutchinson, Kansas salt mines, off limits to all but the lawyers. The Union Pacific currently declines to help with former employee genealogy requests. However, if you are looking for railroad employee records for early Colorado railroads, you may have some success. The Colorado Railroad Museum Library currently has 11,368 employee personnel records. These Colorado employee records are primarily for the following railroads which are not longer operating. Atchison, Topeka & Santa Fe Railroad (AT&SF) Atchison, Topeka and Santa Fe Railroad employee records of employment are recorded in a bound ledger book (record number 736) and box numbers 766 and 1287 for the years 1883 through 1939 for the joint line from Denver to Pueblo.
    [Show full text]
  • Interpretations of Gravity Anomalies at Olympus Mons, Mars: Intrusions, Impact Basins, and Troughs
    Lunar and Planetary Science XXXIII (2002) 2024.pdf INTERPRETATIONS OF GRAVITY ANOMALIES AT OLYMPUS MONS, MARS: INTRUSIONS, IMPACT BASINS, AND TROUGHS. P. J. McGovern, Lunar and Planetary Institute, Houston TX 77058-1113, USA, ([email protected]). Summary. New high-resolution gravity and topography We model the response of the lithosphere to topographic loads data from the Mars Global Surveyor (MGS) mission allow a re- via a thin spherical-shell flexure formulation [9, 12], obtain- ¡g examination of compensation and subsurface structure models ing a model Bouguer gravity anomaly ( bÑ ). The resid- ¡g ¡g ¡g bÓ bÑ in the vicinity of Olympus Mons. ual Bouguer anomaly bÖ (equal to - ) can be Introduction. Olympus Mons is a shield volcano of enor- mapped to topographic relief on a subsurface density interface, using a downward-continuation filter [11]. To account for the mous height (> 20 km) and lateral extent (600-800 km), lo- cated northwest of the Tharsis rise. A scarp with height up presence of a buried basin, we expand the topography of a hole Ö h h ¼ ¼ to 10 km defines the base of the edifice. Lobes of material with radius and depth into spherical harmonics iÐÑ up h with blocky to lineated morphology surround the edifice [1-2]. to degree and order 60. We treat iÐÑ as the initial surface re- Such deposits, known as the Olympus Mons aureole deposits lief, which is compensated by initial relief on the crust mantle =´ µh c Ñ c (hereinafter abbreviated as OMAD), are of greatest extent to boundary of magnitude iÐÑ . These interfaces the north and west of the edifice.
    [Show full text]
  • Meat: a Novel
    University of New Hampshire University of New Hampshire Scholars' Repository Faculty Publications 2019 Meat: A Novel Sergey Belyaev Boris Pilnyak Ronald D. LeBlanc University of New Hampshire, [email protected] Follow this and additional works at: https://scholars.unh.edu/faculty_pubs Recommended Citation Belyaev, Sergey; Pilnyak, Boris; and LeBlanc, Ronald D., "Meat: A Novel" (2019). Faculty Publications. 650. https://scholars.unh.edu/faculty_pubs/650 This Book is brought to you for free and open access by University of New Hampshire Scholars' Repository. It has been accepted for inclusion in Faculty Publications by an authorized administrator of University of New Hampshire Scholars' Repository. For more information, please contact [email protected]. Sergey Belyaev and Boris Pilnyak Meat: A Novel Translated by Ronald D. LeBlanc Table of Contents Acknowledgments . III Note on Translation & Transliteration . IV Meat: A Novel: Text and Context . V Meat: A Novel: Part I . 1 Meat: A Novel: Part II . 56 Meat: A Novel: Part III . 98 Memorandum from the Authors . 157 II Acknowledgments I wish to thank the several friends and colleagues who provided me with assistance, advice, and support during the course of my work on this translation project, especially those who helped me to identify some of the exotic culinary items that are mentioned in the opening section of Part I. They include Lynn Visson, Darra Goldstein, Joyce Toomre, and Viktor Konstantinovich Lanchikov. Valuable translation help with tricky grammatical constructions and idiomatic expressions was provided by Dwight and Liya Roesch, both while they were in Moscow serving as interpreters for the State Department and since their return stateside.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Prime Meridian ×
    This website would like to remind you: Your browser (Apple Safari 4) is out of date. Update your browser for more × security, comfort and the best experience on this site. Encyclopedic Entry prime meridian For the complete encyclopedic entry with media resources, visit: http://education.nationalgeographic.com/encyclopedia/prime-meridian/ The prime meridian is the line of 0 longitude, the starting point for measuring distance both east and west around the Earth. The prime meridian is arbitrary, meaning it could be chosen to be anywhere. Any line of longitude (a meridian) can serve as the 0 longitude line. However, there is an international agreement that the meridian that runs through Greenwich, England, is considered the official prime meridian. Governments did not always agree that the Greenwich meridian was the prime meridian, making navigation over long distances very difficult. Different countries published maps and charts with longitude based on the meridian passing through their capital city. France would publish maps with 0 longitude running through Paris. Cartographers in China would publish maps with 0 longitude running through Beijing. Even different parts of the same country published materials based on local meridians. Finally, at an international convention called by U.S. President Chester Arthur in 1884, representatives from 25 countries agreed to pick a single, standard meridian. They chose the meridian passing through the Royal Observatory in Greenwich, England. The Greenwich Meridian became the international standard for the prime meridian. UTC The prime meridian also sets Coordinated Universal Time (UTC). UTC never changes for daylight savings or anything else. Just as the prime meridian is the standard for longitude, UTC is the standard for time.
    [Show full text]
  • Evidence of Shock Metamorphism Effects in Allochthonous Breccia Deposits from the Colônia Crater, São Paulo, Brazil
    International Journal of Geosciences, 2013, 4, 274-282 http://dx.doi.org/10.4236/ijg.2013.41A025 Published Online January 2013 (http://www.scirp.org/journal/ijg) Evidence of Shock Metamorphism Effects in Allochthonous Breccia Deposits from the Colônia Crater, São Paulo, Brazil Victor F. Velázquez1, Claudio Riccomini2, José M. Azevedo Sobrinho3, Mikhaela A. J. S. Pletsch1, Alethéa E. Martins Sallun3, William Sallun Filho3, Jorge Hachiro2 1Escola de Artes, Ciências e Humanidades, Universidade de São Paulo, São Paulo, Brasil 2Instituto de Geociências, Universidade de São Paulo, São Paulo, Brasil 3Instituto Geológico, Secretaria do Meio Ambiente, São Paulo, Brasil Email: [email protected] Received October 16, 2012; revised November 17, 2012; accepted December 19, 2012 ABSTRACT The 3.6 km-diameter Colônia impact crater, centred at 23˚52'03"S and 46˚42'27"W, lies 40 km to the south-west of the São Paulo city. The structure was formed on the crystalline basement rocks and displays a bowl-shaped with steeper slope near the top that decreases gently toward the centre of the crater. Over recent years were drilled two boreholes inside the crater, which reached a maximum depth of 142 m and 197 m. Geological profile suggests four different lithological associations: 1) unshocked crystalline basement rocks (197 - 140 m); 2) fractured/brecciated basement rocks (140 - 110 m); 3) polymictic allochthonous breccia deposits (110 - 40 m); and 4) post-impact deposits (40 - 0 m). Petrographic characterisation of the polymictic allochthonous breccia reveals a series of distinctive shock-metamorphic features, including, among others, planar deformation features in quartz, feldspar and mica, ballen silica, granular tex- ture in zircon and melt-bearing impact rocks.
    [Show full text]
  • Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J.
    [Show full text]
  • The Co-Evolution of Mars' Atmosphere and Massive South Polar CO2 Ice
    Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6008.pdf 1 1 The Co-Evolution of Mars’ Atmosphere and Massive South Polar CO2 Ice Deposit. P. B. Buhler , S. Piqueux , A. P. Ingersoll2, B. L. Ehlmann1,2, and P. O. Hayne3, 1Jet Propulsion Laboratory, California Institute of Technology ([email protected]), 2 California Institute of Technology, 3University of Colorado Boulder Introduction: A Massive CO2 Ice Deposit (MCID) history from a lookup table of polar insolation as a func- that rivals the mass of Mars’ current, 96% CO2 atmos- tion of orbital elements. phere was recently discovered to overlie part of Mars’ Model Results: H2O Layer Formation. Our model southern H2O cap [1]. The MCID is layered: a top layer predicts that the MCID loses mass during epochs of ris- of 1-10 m of CO2, the Residual South Polar Cap (RSPC) ing polar insolation (Mars’ present state), and gains [2], is underlain by ~10-20 m of H2O ice, followed by mass when insolation falls. H2O ice impurities (~1%) up to three 100s-meter-thick layers of CO2 ice, sepa- also accumulate onto the MCID along with the CO2 ice rated by two layers of ~20-40 m of H2O ice [3] (Fig. 1). in both epochs of rising and falling insolation (Fig. 2). Previous studies invoked orbital cycles to explain the During epochs of rising insolation, the MCID loses ~10- 3 -1 -4 -1 layering, assuming the H2O ice insulates and seals in the m yr CO2, leaving behind impurities (~10 m yr CO2, allowing it to survive periods of high obliquity H2O) that consolidate into a lag layer.
    [Show full text]
  • Bio-Preservation Potential of Sediment in Eberswalde Crater, Mars
    Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Fall 2020 Bio-preservation Potential of Sediment in Eberswalde crater, Mars Cory Hughes Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Hughes, Cory, "Bio-preservation Potential of Sediment in Eberswalde crater, Mars" (2020). WWU Graduate School Collection. 992. https://cedar.wwu.edu/wwuet/992 This Masters Thesis is brought to you for free and open access by the WWU Graduate and Undergraduate Scholarship at Western CEDAR. It has been accepted for inclusion in WWU Graduate School Collection by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. Bio-preservation Potential of Sediment in Eberswalde crater, Mars By Cory M. Hughes Accepted in Partial Completion of the Requirements for the Degree Master of Science ADVISORY COMMITTEE Dr. Melissa Rice, Chair Dr. Charles Barnhart Dr. Brady Foreman Dr. Allison Pfeiffer GRADUATE SCHOOL David L. Patrick, Dean Master’s Thesis In presenting this thesis in partial fulfillment of the requirements for a master’s degree at Western Washington University, I grant to Western Washington University the non-exclusive royalty-free right to archive, reproduce, distribute, and display the thesis in any and all forms, including electronic format, via any digital library mechanisms maintained by WWU. I represent and warrant this is my original work, and does not infringe or violate any rights of others. I warrant that I have obtained written permissions from the owner of any third party copyrighted material included in these files.
    [Show full text]
  • Ancient Fluid Escape and Related Features in Equatorial Arabia Terra (Mars)
    EPSC Abstracts Vol. 7 EPSC2012-132-3 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 Ancient fluid escape and related features in equatorial Arabia Terra (Mars) F. Franchi(1), A. P. Rossi(2), M. Pondrelli(3), B. Cavalazzi(1), R. Barbieri(1), Dipartimento di Scienze della Terra e Geologico Ambientali, Università di Bologna, via Zamboni 67, 40129 Bologna, Italy ([email protected]). 2Jacobs University, Bremen, Germany. 3IRSPS, Università D’Annunzio, Pescara, Italy. Abstract Noachian [1]. The ELDs are composed by light rocks showing a polygonal pattern, described elsewhere on Arabia Terra, in the equatorial region of Mars, is Mars [4], and is characterized by a high sinuosity of long-time studied area especially for the abundance the strata that locally follows a concentric trend of fluid related features. Detailed stratigraphic and informally called “pool and rim” structures (Fig. morphological study of the succession exposed in the 1A). Crommelin and Firsoff craters evidenced the occurrences of flow structures and spring deposits that endorse the presence of fluids circulation in the Late Noachian. All the morphologies in these two proto-basins occur within the Equatorial Layered Deposits (ELDs). 1. Introduction Martian layered spring deposits are of considerable interest for their supposed relationship with water and high potential of microbial signatures preservation. Their supposed fluid-related origin [1] makes the Equatorial Layered Deposits attractive targets for future missions with astrobiological purposes. In this study we report the occurrence of mounds fields and flow structures in Firsoff and Crommelin craters and summarize the result of a detailed study of the remote-sensing data sets available in this region.
    [Show full text]
  • Downloaded for Personal Non-Commercial Research Or Study, Without Prior Permission Or Charge
    MacArtney, Adrienne (2018) Atmosphere crust coupling and carbon sequestration on early Mars. PhD thesis. http://theses.gla.ac.uk/9006/ Copyright and moral rights for this work are retained by the author A copy can be downloaded for personal non-commercial research or study, without prior permission or charge This work cannot be reproduced or quoted extensively from without first obtaining permission in writing from the author The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the author When referring to this work, full bibliographic details including the author, title, awarding institution and date of the thesis must be given Enlighten:Theses http://theses.gla.ac.uk/ [email protected] ATMOSPHERE - CRUST COUPLING AND CARBON SEQUESTRATION ON EARLY MARS By Adrienne MacArtney B.Sc. (Honours) Geosciences, Open University, 2013. Submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy at the UNIVERSITY OF GLASGOW 2018 © Adrienne MacArtney All rights reserved. The author herby grants to the University of Glasgow permission to reproduce and redistribute publicly paper and electronic copies of this thesis document in whole or in any part in any medium now known or hereafter created. Signature of Author: 16th January 2018 Abstract Evidence exists for great volumes of water on early Mars. Liquid surface water requires a much denser atmosphere than modern Mars possesses, probably predominantly composed of CO2. Such significant volumes of CO2 and water in the presence of basalt should have produced vast concentrations of carbonate minerals, yet little carbonate has been discovered thus far.
    [Show full text]