DOCSLIB.ORG

O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System RADAR ALTIMETRY of the LARGE ?.LARTIAN CRATERS

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System RADAR ALTIMETRY of the LARGE ?.LARTIAN CRATERS RADAR ALTIMETRY OF THE LARGE MARTIAN CRATERS, L. E. Roth, G. S. Downs, and R. S. Saunders, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91103; G. Schubert, Department of Earth and Space Sciences, University of California, Los Angeles, California 90024. The Goldstone Mars data (1,2) have been used to obtain detailed morpho- metric information on martian craters. Some qualitative results of this effort have been reported previously (3). Radar profiles of a total of 131 impact craters have been recognized. (The following symbols are used in the subsequent discussion: Ri (km) is crater depth and Dr (km) is rim-crest diameter (4)). The craters range in size from Dr " 20 km to Dr " 500 km, and are all located within a subequatorial belt of the cratered highlands, bounded by approximate latitudes of -14' and -21'. This belt constitutes about 8% of the total surface area of the planet. The current data coverage does not exceed approximately 25% of the area of the belt, i.e., about 2% of the area of the planet. Radar profiles of large craters with the visually flat floors show sub- dued crater rims (rarely higher than 300-400 meters), usually shallow interior walls, and little structural detail in the interior and the exterior walls. In contrast, the floors of the same craters often display topographic relief greater than the error in the range measurement. The largest craters (Dr > 125 km) show differing degrees of the floor level adjustment. The two extreme cases are the craters Bakhuysen (Dr = 140 km, (-23.0°, 344.0')) whose floor is almost 2500 m below the surrounding terrain, in sharp contrast with Denning (Dr = 140 km, (-17.8O, 326.5O)) whose floor is almost at the same level as the surrounding terrain. Depths of the scanned craters have been determined with varying degrees of confidence. The data confirm the overall shallowness of themartiancraters, an observation made as early as the time of Mariner 4 and since then noted by several investigators (4-10). The measured radar depths of most of the 87 objects comprising the higher-confidence grouping cluster between 1 krn and 2 km. Ca~sequ$ntly, the least-squares fit to the relationship of the log depth versus the log diameter, is markedly less steep than a similar curve derived from the Mariner 9 UVS altimetry (7). Thus the depths of a mixed degradation stateandgeographically (D > 20 km)areonlyaweak function restricted radar sample of martian craters r of diameter. If the crater depth measurements are split into two subgroups, one with diameters less than 125 km and the other with diameters greater than 125 km, and the depthldiameter ratios for each subgrobp are fitted in the least-squares sense, a pronounced break in slope, a "knee," at the junction of both fits can be observed. Since the 125 km diameter division was arbitrarily chosen,wecannot be sure that a knee in the depthldiameter relation,actually occurs at this diameter. However, these results do suggest that a knee exists somewhere in the diameter range from 100 km to 200 km. It is seen that for Dr > 125 km the average depths of ;th_e sampled martian craters become virtually independent of the crater size. , Therefore, a power-law least-squares fit of the depth/ .* - %. O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System RADAR ALTIMETRY OF THE LARGE ?.LARTIAN CRATERS Roth, L. E. et al. diameter relationship for a mixed-age crater population, taken over the full range of diameters obsc.ures a possibly significant change in the depthldia- meter curve for Mars. It sllouldbenoted, however, that confidence in the accuracy of the radar range measurements decreases as the dimensions of the measured object become comparable to the dimensions of the radar footprint. Thus the least-squares fits in Eqs. (1) and (2) may suffer fromcontamination by the less reliable data points, while Eq. (3) gives abetterrepresentation of the depth/diameter relationship for the largemartiancraters. Clarifica- tion of this matter will have to be postponed until more dataareavailable. Because of the proximity of the radar depth/diameter curve to the lower boundary of the envelope containing the depth/diameter ratios of Pre-Imbrian lunar craters (5,7) it has to be concluded that the large martian craters contained in the radar compilation are substantially shallower and hence sub- stantially more modified than the lunar cratersofcorresponding age and size. This should come as no surprise since the martian craters appear to have been excavated to shallower depths (10) and have unquestionably been exposed to a more erosive environment and a more vigorous gravitational settling. In addition, the radar results show certain large martian craters to have been modified by some processesthattiltedthecrater floorsrelativeto the hori- zontal plane, thus enhancingtheir shallowvisual appearance. Themost prominent among the craters with tilted floors are Gusev (Dr = 170 km, Ri = 1.6 km, (-14.7O, 184.5')) and Williams (Dr = 125 km, Ri = 8 km, (-18.00, 164.0')). Gusev is located within the range of the Apollinaris Patera lava flows, andit serves as a terminus of the Ma'adim Vallis. The floor tilt may thus be related to the filling history of the crater. Williams is locatedatthe foot of the eastward-facing fault blocks in Memnonia (11) and its floor tilt isapparently associated with the regional tectonic trends. The Apollo Lunar Sounder radar images revealed the centers of the floors of some large lunar craters to be domed upward by several hundred meters. No such effect has been observed in the Coldstone Hars data. The shallow depths of the large martian craters, the modest slope ofthe depth/diameter curve at large diameters, and the absence of crater floor doming can be interpreted in several ways: (1) Compared to their lunar counterparts, the large martian craters have undergone a more complete post- impact structural adjustment. As a result, the doming, presumably an inter- mediate phase in such a process, has vanished and the floors of the large martian craters are structurally flat. (2) The large martian craters have retained a structural bulge, but it has been obliterated by a blanket of eolian/fluvial/volcanic deposits. If the latter is true, then modification by erosion and deposition is a significant process of landform and crater degradation on Mars. (3) The shallow initial depths remain the dominant fac- tor in the evolution of large martian craters, while the post-impact modifi- cation by pr.ocesses listed above is of secondary importance. References: (1) Downs, G. S., Goldstein, R. M., Green, R. R., Morris, G. A., and Reichley, P. E. (1973). --Icarus 18, 8-21; (2) Downs, G. S., Reichley, P. E., and Green, R. R. (1975). Icarus 26, 273-312; (3) Roth, L. E., Elachi, C., Saunders, R. S., and Schubert, G. (1978). Lunar and Planetary Science -IX, 976-978; (4) Pike, R. J. (1974). Geophys. Res. Lett. 1, 291-294; (5) Pike, R. J. (1971). Icarus 19, 384-395; (6) Burt, T., ~everka,T., and Cook, K. (1976). --Icarus 29, 83-90; (7) Cintala, M. J. et al. (1976). Proc. Lunar Sci. Conf. a,3575-3587; (8) Malin, M. D. et al. (1977). J. Geophys. Res. -82, 376-388; i'F) Schubert, G. et al. (1977). Icarus 32, 131-146;(10)~intala, If. J and Mouginis--Mark, P J. (1980), Geophys, Res. Lett. 7, 329-332; (11) Plescia, J. B. et al. (1980). Lunar and Plan. Sci. a,891-893. O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System .
Load more

Recommended publications
  • 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]
  • MDRS Final Summary Report – Crew 78 Vincent Beaudry, Kathryn Denning, Judah Epstein, Dirk Geeroms, Balwant Rai, Grier Wilt
    MDRS final summary report – Crew 78 Vincent Beaudry, Kathryn Denning, Judah Epstein, Dirk Geeroms, Balwant Rai, Grier Wilt Introduction If interplanetary colonization is to be possible, humanity needs to learn as much as possible about how to rise to the challenges involved. One way to achieve this is, of course, through simulations. Our crew, the 78th in the Mars Desert Research Station simulation, was intensively international, composed of 2 Canadians (Kathryn Denning, Vincent Beaudry), 2 Americans (Judah Epstein, Grier Wilt), one Belgian (Dirk Geeroms) and one Indian (Balwant Rai). None of us had met before, and joining together to overcome language barriers and explore cultural differences provided us with an intense intercultural experience, surely akin to those which will be a part of future space exploration. As a group, we: developed our own knowledge of the challenges of space exploration; contributed to some ongoing MDRS research into extremophiles, environmental impact, and plant growth; furthered our individual projects in human physiology, long-distance teaching, and anthropology; acted as subjects for outside human factors researchers; and worked together to make life at the Hab go smoothly, including making some improvements to the Hab and to the EVA equipment. The Group Our crew was comprised of 6 individuals, with the following specialties: Vincent Beaudry was the commander, Judah Epstein the engineer and executive officer, Balwant Rai the scientist and health and security officer, Grier Wilt our biologist, Dirk Geeroms the teacher and astronomer, and Kathryn Denning our anthropologist and journalist. Although we all had our respective roles within this two weeks journey, we all enjoyed very much taking part in each others experiences and in the everyday tasks.
    [Show full text]
  • Ancient Geodynamics and Global-Scale Hydrology on Mars
    R EPORTS ␪ 15. ccs represents the CO2 concentration at the chloro- component and calculate eq from a weighting of plast surface, which is the limit of CA activity and is 75:25 C4 grasses:trees to allow for the presence of thus assumed to represent the site of CO2-H2Oin trees in savanna-type habitats. Group 9 (C3 grassland leaves. ccs is typically a midway value between those and agriculture) we assume comprises 25:50:25 for in the liquid-air interfaces and the sites of CO2 trees:C3 grasses:C4 grasses; the C3 and C4 grasses assimilation inside leaves (14). include some C3 herbs and C4 grass species as crops. 16. Supplementary data are available on Science Online 31. G. Hoffmann et al., in preparation. at www.sciencemag.org/cgi/content/full/291/5513/ 32. J. R. Ehleringer, T. E. Cerling, B. R. Helliker, Oecologia 2584/DC1. 112, 285 (1997). 17. M. D. Hatch, J. N. Burnell, Plant Physiol. 93, 825 33. G. J. Collatz, J. A. Berry, J. S. Clark, Oecologia 114, 441 (1990). (1998). 18. E. Utsoniyama, S. Muto, Physiol. Plant. 88, 413 34. J. Lloyd, G. D. Farquhar, Oecologia 99, 201 (1994). (1993). 35. M. Trolier, J. W. C. White, J. R. Lawrence, W. S. 19. A. Makino et al., Plant Physiol. 100, 1737 (1992) Broecker, J. Geophys. Res. 101, 25897 (1996). 20. G. A. Mills, H. C. Urey, J. Am. Chem. Soc. 62, 1019 36. R. A. Houghton, Tellus 51B, 298 (1999). (1940). 37. R. H. Waring, W. H. Schlesinger, Forest Ecosystems 21. J. S.
    [Show full text]
  • 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
    [Show full text]
  • The Pueblo in the Mojave Sink: an Archaeological Myth
    California State University, San Bernardino CSUSB ScholarWorks Theses Digitization Project John M. Pfau Library 2002 The pueblo in the Mojave Sink: An archaeological myth Barbara Ann Loren-Webb Follow this and additional works at: https://scholarworks.lib.csusb.edu/etd-project Part of the Archaeological Anthropology Commons Recommended Citation Loren-Webb, Barbara Ann, "The pueblo in the Mojave Sink: An archaeological myth" (2002). Theses Digitization Project. 2107. https://scholarworks.lib.csusb.edu/etd-project/2107 This Thesis is brought to you for free and open access by the John M. Pfau Library at CSUSB ScholarWorks. It has been accepted for inclusion in Theses Digitization Project by an authorized administrator of CSUSB ScholarWorks. For more information, please contact [email protected]. THE PUEBLO IN THE MOJAVE SINK: AN ARCHAEOLOGICAL MYTH A Thesis Presented to the Faculty of California State University, San Bernardino In Partial Fulfillment of the Requirements for the Degree Masters of Arts in Interdisciplinary Studies by Barbara Ann Loren-Webb March 2003 THE PUEBLO IN THE MOJAVE SINK: AN ARCHAEOLOGICAL MYTH A Thesis Presented to the Faculty of California State University, San Bernardino by Barbara Ann Loren-Webb March 2003 Approved by: Russell Barber, Chair, Anthropology Date Pete Robertshesw, Anthropology ABSTRACT In 1929 Malcolm Rogers published a paper in which he stated that there was evidence of an Anasazi or Puebloan settlement or pueblo, in the Mojave Sink Region of the Mojave Desert. Since then, archaeologists have cited Rogers' publication and repeated his claim that such a pueblo was located in the Western Mojave Desert. The purpose of this thesis started out as a review of the existing evidence and to locate this pueblo.
    [Show full text]
  • Ebook < Impact Craters on Mars # Download
    7QJ1F2HIVR # Impact craters on Mars « Doc Impact craters on Mars By - Reference Series Books LLC Mrz 2012, 2012. Taschenbuch. Book Condition: Neu. 254x192x10 mm. This item is printed on demand - Print on Demand Neuware - Source: Wikipedia. Pages: 50. Chapters: List of craters on Mars: A-L, List of craters on Mars: M-Z, Ross Crater, Hellas Planitia, Victoria, Endurance, Eberswalde, Eagle, Endeavour, Gusev, Mariner, Hale, Tooting, Zunil, Yuty, Miyamoto, Holden, Oudemans, Lyot, Becquerel, Aram Chaos, Nicholson, Columbus, Henry, Erebus, Schiaparelli, Jezero, Bonneville, Gale, Rampart crater, Ptolemaeus, Nereus, Zumba, Huygens, Moreux, Galle, Antoniadi, Vostok, Wislicenus, Penticton, Russell, Tikhonravov, Newton, Dinorwic, Airy-0, Mojave, Virrat, Vernal, Koga, Secchi, Pedestal crater, Beagle, List of catenae on Mars, Santa Maria, Denning, Caxias, Sripur, Llanesco, Tugaske, Heimdal, Nhill, Beer, Brashear Crater, Cassini, Mädler, Terby, Vishniac, Asimov, Emma Dean, Iazu, Lomonosov, Fram, Lowell, Ritchey, Dawes, Atlantis basin, Bouguer Crater, Hutton, Reuyl, Porter, Molesworth, Cerulli, Heinlein, Lockyer, Kepler, Kunowsky, Milankovic, Korolev, Canso, Herschel, Escalante, Proctor, Davies, Boeddicker, Flaugergues, Persbo, Crivitz, Saheki, Crommlin, Sibu, Bernard, Gold, Kinkora, Trouvelot, Orson Welles, Dromore, Philips, Tractus Catena, Lod, Bok, Stokes, Pickering, Eddie, Curie, Bonestell, Hartwig, Schaeberle, Bond, Pettit, Fesenkov, Púnsk, Dejnev, Maunder, Mohawk, Green, Tycho Brahe, Arandas, Pangboche, Arago, Semeykin, Pasteur, Rabe, Sagan, Thira, Gilbert, Arkhangelsky, Burroughs, Kaiser, Spallanzani, Galdakao, Baltisk, Bacolor, Timbuktu,... READ ONLINE [ 7.66 MB ] Reviews If you need to adding benefit, a must buy book. Better then never, though i am quite late in start reading this one. I discovered this publication from my i and dad advised this pdf to find out. -- Mrs. Glenda Rodriguez A brand new e-book with a new viewpoint.
    [Show full text]
  • NAC Planetary Protection Subcommittee, December 8-9, 2015
    NAC Planetary Protection Subcommittee, December 8-9, 2015 NASA ADVISORY COUNCIL Planetary Protection Subcommittee December 8-9, 2015 NASA Headquarters Washington, D.C. MEETING MINUTES _____________________________________________________________ Robert Lindberg, Chair ____________________________________________________________ Amy Kaminski, Executive Secretary Report prepared by Joan M. Zimmermann Zantech IT, Inc. 1 NAC Planetary Protection Subcommittee, December 8-9, 2015 Table of Contents Introduction 3 Words from the Chair 3 Discussion with Science Mission Directorate Associate Administrator 3 Planetary Protection Issues and Updates 5 Planetary Science Division Update 7 Mars Exploration Program Update 9 Committee on Space Research (COSPAR) Panel Colloquium - Mars Special Regions 11 - Icy Worlds 13 Meeting with European Space Agency’s Planetary Protection Working Group 13 MSL Gale Crater Observations 15 Mars 2020 Planetary Protection Requirements 16 Public Comment 18 Returned Sample Science Board 18 Mars 2020 Planetary Protection – Jet Propulsion Laboratory Briefing 20 Public Comment 27 Findings and Recommendations Discussion 27 Appendix A- Attendees Appendix B- Membership roster Appendix C- Presentations Appendix D- Agenda 2 NAC Planetary Protection Subcommittee, December 8-9, 2015 December 8, 2015 Introduction NASA Advisory Council (NAC) Planetary Protection Subcommittee (PPS) Chair, Dr. Robert Lindberg, opened the meeting. The Executive Secretary of the PPS, Dr. Amy Kaminski, made preparatory and logistical announcements. Introductions were made around the room. Words from the Chair Dr. Lindberg welcomed members to the meeting, and disclosed for purposes of transparency that he had recently taken a new position that has some relevance to planetary protection (PP), as Vice President for Orbital and Return Systems for Moon Express, a commercial entity that will be pursuing exploration and mining on the Moon.
    [Show full text]
  • Structure, Stratigraphy, and Origin of Husband Hill, Columbia Hills, Gusev Crater, Mars T
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113, E06S03, doi:10.1029/2007JE003041, 2008 Click Here for Full Article Structure, stratigraphy, and origin of Husband Hill, Columbia Hills, Gusev Crater, Mars T. J. McCoy,1 M. Sims,2 M. E. Schmidt,1 L. Edwards,2 L. L. Tornabene,3 L. S. Crumpler,4 B. A. Cohen,5 L. A. Soderblom,6 D. L. Blaney,7 S. W. Squyres,8 R. E. Arvidson,9 J. W. Rice Jr.,10 E. Tre´guier,11 C. d’Uston,11 J. A. Grant,12 H. Y. McSween Jr.,13 M. P. Golombek,7 A. F. C. Haldemann,14 and P. A. de Souza Jr.15,16 Received 15 November 2007; revised 26 February 2008; accepted 7 April 2008; published 17 June 2008. [1] The strike and dip of lithologic units imaged in stereo by the Spirit rover in the Columbia Hills using three-dimensional imaging software shows that measured dips (15– 32°) for bedding on the main edifice of the Columbia Hill are steeper than local topography (8–10°). Outcrops measured on West Spur are conformable in strike with shallower dips (7–15°) than observed on Husband Hill. Dips are consistent with observed strata draping the Columbia Hills. Initial uplift was likely related either to the formation of the Gusev Crater central peak or ring or through mutual interference of overlapping crater rims. Uplift was followed by subsequent draping by a series of impact and volcaniclastic materials that experienced temporally and spatially variable aqueous infiltration, cementation, and alteration episodically during or after deposition. West Spur likely represents a spatially isolated depositional event.
    [Show full text]
  • Evidence of Redox Sensitive Elements Associated with Possible Shoreline Sediments in Gale Crater
    49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2483.pdf EVIDENCE OF REDOX SENSITIVE ELEMENTS ASSOCIATED WITH POSSIBLE SHORELINE SEDIMENTS IN GALE CRATER. P. J. Gasda ([email protected])1, N. L. Lanza1, S. N. Lamm2, J. L’Haridon3, P.- Y. Meslin4, O. Forni4, J. Frydenvang5, N. Stein6, W. Fischer6, F. Rivera-Hernandez7, H. E. Newsom8, B. Clark9, R. C. Wiens1, S. M. Clegg1, S. Maurice4; 1LANL, 2KSU, 3U. Nantes, 4IRAP, 5U. Copenhagen, Nat Hist Museum, 6Caltech, 7UC Davis, 8UNM, 9SSI Introduction: Over 5 years of investigating Gale range of phosphate species [e.g., 21]. On Earth, these crater, NASA’s Curiosity rover has revealed that the shallow water environments become oxidizing through crater once hosted a habitable stratified lake fed by contact with an oxidizing atmosphere. rivers and streams [1–4]. Even as the lake disappeared Chemical observations: Overall, the Murray fm. and lake sediment was buried by eolian deposits and has a low abundance of Mn. However, there is a sub- exhumed multiple times, multiple episodes of ground- stantial increase in Mn found in the bedrock at eleva- water circulated through fractures that formed within tions -4275– -4340 m (Fig. 1). For example, the target the ancient lakebed deposits (informally the “Murray” Newport Ledge contains ~6.4–11.5 wt% MnO (shot formation), transporting Ca sulfate, silica, borate, Fe, averaged) (Fig. 2). The target Denning Brook (Fig. 3) and Mn and prolonging habitable conditions [5–8]. is P-rich and contains ~2.3–16 wt% MnO (shot aver- Recent chemical and sedimentological observations aged). These dark-toned deposits typically have higher from sols ~1520–1800 are consistent with potential MnO and FeO than nearby light-toned targets and temporary shoreline environments where ChemCam lower SiO2, Al2O3, and K2O.
    [Show full text]
  • Topographic Map of Mars
    U.S. DEPARTMENT OF THE INTERIOR OPEN-FILE REPORT 02-282 U.S. GEOLOGICAL SURVEY Prepared for the NATIONAL AERONAUTICS AND SPACE ADMINISTRATION 180° 0° 55° –55° Russell Stokes 150°E NOACHIS 30°E 210°W 330°W 210°E NOTES ON BASE smooth global color look-up table. Note that the chosen color scheme simply 330°E Darwin 150°W This map is based on data from the Mars Orbiter Laser Altimeter (MOLA) 30°W — 60° represents elevation changes and is not intended to imply anything about –60° Chalcoporous v (Smith and others 2001), an instrument on NASA’s Mars Global Surveyor Milankovic surface characteristics (e.g. past or current presence of water or ice). These two (MGS) spacecraft (Albee and others 2001). The image used for the base of this files were then merged and scaled to 1:25 million for the Mercator portion and Rupes map represents more than 600 million measurements gathered between 1999 1:15,196,708 for the two Polar Stereographic portions, with a resolution of 300 and 2001, adjusted for consistency (Neumann and others 2001 and 2002) and S dots per inch. The projections have a common scale of 1:13,923,113 at ±56° TIA E T converted to planetary radii. These have been converted to elevations above the latitude. N S B LANI O A O areoid as determined from a martian gravity field solution GMM2 (Lemoine Wegener a R M S s T u and others 2001), truncated to degree and order 50, and oriented according to IS s NOMENCLATURE y I E t e M i current standards (see below).
    [Show full text]
  • Mojave Trails National Monument Proposal
    28 36 62 Mojave Trails National 3 66 China Lake Naval Air Death Valley National Park 10 Monument Proposal Weapons Center 41 1 11 Ivanpah Bright Source Solar Project Ridgecrest 60 12 71 9 17 23 Proposed Mojave Trails National Monument Route 66 (National Trails Highway) Solar Millennium Ridgecrest Solar Project (941,000 acres) 33 32 Catellus lands account for 199,613 acres within County Boundary Spangler Hills 65 monument boundary OHV Area 17 4 Proposed Wild and Scenic River 14 Administrative/Ownership Summary of Lands Within the China Lake Proposed Mojave Trails National Monument: (in acres) 6 Naval Air 37 ACEC...................................................................................468,672 47 Renewable Energy Action Team (2,720,000 acres) 27 Weapons Center 29 Cady Mountains WSA...........................................................84,000 77 Catellus lands outside ACEC boundaries.............................103,221 5 27 Fort Irwin Other BLM Lands...............................................................285,520 BLM Solar Study Area (351,000 acres) 27 60 Of these lands less than 75,000 are less than 5% slope 27 69 NTC 8 State Lands..........................................................................32,168 Private Lands.......................................................................72,125 Fast-Track Renewable Energy Projects 27 78 70 27 6 Sand to Snow National Monument 27 25 Baker Proposed Sand to Snow National Monument (134,000 acres) 27 10 76 27 Proposed Congressionally Approved Off Highway Vehicle Areas 76
    [Show full text]
  • Game Program
    lrbears.com @BearsSports #GOBEARS BEARS vs. BARTON GAMEDAY MARCH 20, 2021 | 4 PM | MORETZ STADIUM LENOIR-RHYNE FOOTBALL MATCHUP 2020-21 Record . 1-0 0-2 . .2019 Record Conference Record . 1-0 0-1 . Conference Record 2019 Postseason Finish . NCAA Quarterfinal None . .2019 Postseason Finish Nickname . Bears Bulldogs . Nickname Location . Hickory, N.C. Wilson, N.C. .. Location Head Coach . Mike Jacobs (1st Season) Chip Hester (1st season) . .Head Coach Conference Affiliation . South Atlantic South Atlantic . .. Conference Affiliation NOTES • The 101st season in Lenoir-Rhyne Football history is one like no other. For the first time ever, the Bears will compete in spring games and today serves as the 2020-21 home opener. The four-game regular season slate concludes with a home game against Catawba on April 10. Should the Bears advance to the SAC Champion- ship game, that will be played on April 17. • Lenoir-Rhyne has won 18 straight games against South Atlantic Conference opponents with two of those wins coming in the NCAA Playoffs. The last loss to a SAC foe came back on Nov. 11, 2017 when the Bears dropped a 24-20 contest at Catawba. • This is the first LR home game since Dec. 7, 2019 in the NCAA Quarterfinal. • LR hasn’t lost a regular season home game since a last-second loss at No. 12 West Alabama on August 30, 2018. The Bears have won 22 straight regular seaso ngames and haven’t lost in the regular season in 932 days. • The Bears and Barton haven’t met since 1950. Barton, who then competed as Atlantic Christian, has never beaten Lenoir-Rhyne.
    [Show full text]