DOCSLIB.ORG

Martian Spherule Size Distribution Between Eagle and Endurance Craters from Opportunity Rover Mi Images

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Martian Spherule Size Distribution Between Eagle and Endurance Craters from Opportunity Rover Mi Images 45th Lunar and Planetary Science Conference (2014) 2026.pdf MARTIAN SPHERULE SIZE DISTRIBUTION BETWEEN EAGLE AND ENDURANCE CRATERS FROM OPPORTUNITY ROVER MI IMAGES. D. Jones1, W. M. Calvin1, P. DeSouza2, and B.L. Joliff3, 1University of Nevada Reno, Reno, NV, USA ([email protected]), 2CSIRO, Private Bag 12, Hobart TAS 7001, Australia, 3Washington University, St. Louis, MO Introduction: The Mars Exploration Rover These include ‘blueberries’, the normal uncoated (MER)-B, Opportunity, landed in Eagle crater within spherules and ‘batter-berries’ which are spherules coat- the Meridiani Planum on January 25, 2004 and began ed with a sulfate-rich outcrop material [4]. ‘Newber- collecting images of rocks and soil with its high resolu- ries’ are observed near Endeavour crater at a target tion Microscopic Imager (MI) [1]. At the time of the known as “Kirkwood” and appear to have a different meeting, Opportunity will have been active on Mars internal structure and composition [7]. for over 10 years, and more than 500 martian sols; traversing over 38 km of Meridiani Planum from Ea- Table 1: Summary of data collected ever each campaign. gle to Endeavour crater. The presence of hematite had been identified from orbit [2]; however, the occurrence of hematite spherules, dubbed ‘blueberries’ by the MER team, was unexpected [3]. Observations support the interpretation that the spherules likely formed as concretions in a more or less homogeneous diffusion setting with no strong directional groundwater flow, but other explanations are possible [3,4,5]. Previous work regarding these spherules has focused primarily on the initial half of Opportunity’s traverse; working both to characterize their nature and origin as well as their size, distribution and chemistry [5,6]. MI image stacks have now been collected on ap- proximately 485 sols on the way to Endeavour crater Data from the alpha particle X-ray spectrometer and an effort was made to examine each of these sols (APXS) shows that the chemical composition of these and measure the diameter of spherules when present. new spherules is not hematite dominant and they may Typically a single image was chosen from each sol for have different origins as well [7]. These ‘new-berries’ measurement based on a selection criteria including: appear to be similar in composition to spherules ob- image/stack quantity, image resolution, number of served by the Spirit Rover (MER-A), at sites such as spherules present, and the number of exposed vs. semi- King George (sol 1035). Diameter measurements in- buried spherules. Perpendicular diameter measure- cluded in this study are primarily of the common ments were made on up to six spherules from each im- ‘blueberry’ type, however some measurements of the age, amounting to just over 750 individual spherules new type have also been included for a broader look at between sols 10 and 3502 as shown in Table 1. Meas- the overall Meridiani spherule size distribution. urements were initially made in pixels, and were then converted to millimeters using a conversion factor of 31 micrometers per pixel [1]. Data obtained over Opportunity’s traverse was seg- regated into 13 separate campaigns based on location; typically, whether close to a significant crater or simply on the plains. The size and number of spherules in each MI location were variable. Target viewing angles also differed in each location. Images in the plains are typically vertically oriented and viewed the surface sediment and eroded-out or partially exposed spher- ules. At craters, the MI was occasionally able to view Figure 1: Examples of the spherule types including exposed horizontal beds and view the spherules within typical ‘blueberries’ in soils near Eagle crater (left) as their sedimentary host rock. well as the ‘new-berries’ seen near Endeavour (right). Three broad distinctions have been previously These full MI image frames are ~ 3.2 cm wide. made to describe the spherules seen at Meridiani. 45th Lunar and Planetary Science Conference (2014) 2026.pdf Figures 2 and 3 show the derived size distributions. south from Endurance crater toward Victoria crater. When possible, measurements focused on including the Another goal of this study was to try and determine largest and smallest spherules seen in each image, with whether proximity to a crater corresponds to any the intention of obtaining the widest range of the size change in the size distribution or relative abundance of distribution. The diameters of measured spherules spherules or if other trends occur in the longer traverse ranged from 0.6 mm to 7.2 mm in size and an estimate distances. However after examining the data in sepa- of the mean diameter was determined to be 2.13 mm, rate campaigns there does not appear to be significant as shown in Table 2. Figure 2 shows the range of sizes size variation near craters in the spherules seen on the in each campaign location and Figure 3 summarizes surface or in outcrop. A slight increase in spherule size sizes for the entire traverse from Eagle to Endeavor. may occur near large craters; however the evidence is The overall distribution is reasonably well-fit by a log- ambiguous. Further research could be done on the normal curve; however the distribution may also be spherules observed by Spirit, not only to further con- bimodal. Since only the largest and smallest spherules strain the size and distribution of martian spherules, but in each image were measured, the distribution curve also understand the nature of spherules on Mars. Very represents the range of sizes rather than the true statis- small spherules, interpreted as impact spherules have tical variation of the size range. been reported at the MSL landing site [8]. Table 2: Descriptive statistics of spherule diameter meas- urements in millimeters. References: [1] Herkenhoff K. E., et al., Science, 1727-1730, 10.1126/science.1105286 (2004). [2] Christensen P. R., et al. J. Geophys. Res., 105, 9623–9642, 10.1029/1999 JE001093 (2000). [3] Squyres S.W., et al. Science, 306(5702), 1709–1714, 10.1126/science.1104559 (2004). [4] McLennan S.M. Figure 2: Box plots showing the distribution of spherule et al. Earth Planet. Sci. Lett. 240, 1, 95-121 10.1016/ measurements from each campaign. Extremes in each loca- j.epsl.2005.09.041 (2005). [5] Calvin W.M. et al. tion are noted by *. (2008) J. Geophys. Res., 113, E12S37, 10.1029/2007JE003048. [6] Joliff B. L. et al., 7th Intl Conf. Mars, #3374. [7] Arvidson R.E., et al. (2014) Science, in press. [8] Yingst A. L., et al. (2013) 44th LPSC, #1257. Figure 3: Spherule size distribution from 1436 individu- al diameter measurements, shown with a lognormal fit. Our results are generally consistent with those of Calvin et al. [5], who measured spherules from early in the mission, but a wider range of sizes in each MI im- age. They noted a general decrease in spherule size .
Load more

Recommended publications
  • Educator's Guide
    EDUCATOR’S GUIDE ABOUT THE FILM Dear Educator, “ROVING MARS”is an exciting adventure that This movie details the development of Spirit and follows the journey of NASA’s Mars Exploration Opportunity from their assembly through their Rovers through the eyes of scientists and engineers fantastic discoveries, discoveries that have set the at the Jet Propulsion Laboratory and Steve Squyres, pace for a whole new era of Mars exploration: from the lead science investigator from Cornell University. the search for habitats to the search for past or present Their collective dream of Mars exploration came life… and maybe even to human exploration one day. true when two rovers landed on Mars and began Having lasted many times longer than their original their scientific quest to understand whether Mars plan of 90 Martian days (sols), Spirit and Opportunity ever could have been a habitat for life. have confirmed that water persisted on Mars, and Since the 1960s, when humans began sending the that a Martian habitat for life is a possibility. While first tentative interplanetary probes out into the solar they continue their studies, what lies ahead are system, two-thirds of all missions to Mars have NASA missions that not only “follow the water” on failed. The technical challenges are tremendous: Mars, but also “follow the carbon,” a building block building robots that can withstand the tremendous of life. In the next decade, precision landers and shaking of launch; six months in the deep cold of rovers may even search for evidence of life itself, space; a hurtling descent through the atmosphere either signs of past microbial life in the rock record (going from 10,000 miles per hour to 0 in only six or signs of past or present life where reserves of minutes!); bouncing as high as a three-story building water ice lie beneath the Martian surface today.
    [Show full text]
  • Exploration of Victoria Crater by the Mars Rover Opportunity
    Exploration of Victoria Crater by the Mars Rover Opportunity The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Squyres, Steven W., Andrew H. Knoll, Raymond E. Arvidson, James W. Ashley, James F. III Bell, Wendy M. Calvin, Philip R. Christensen, et al. 2009. Exploration of Victoria Crater by the Mars rover Opportunity. Science 324(5930): 1058-1061. Published Version doi:10.1126/science.1170355 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:3934552 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP Exploration of Victoria Crater by the Rover Opportunity S.W. Squyres1, A.H. Knoll2, R.E. Arvidson3, J.W. Ashley4, J.F. Bell III1, W.M. Calvin5, P.R. Christensen4, B.C. Clark6, B.A. Cohen7, P.A. de Souza Jr.8, L. Edgar9, W.H. Farrand10, I. Fleischer11, R. Gellert12, M.P. Golombek13, J. Grant14, J. Grotzinger9, A. Hayes9, K.E. Herkenhoff15, J.R. Johnson15, B. Jolliff3, G. Klingelhöfer11, A. Knudson4, R. Li16, T.J. McCoy17, S.M. McLennan18, D.W. Ming19, D.W. Mittlefehldt19, R.V. Morris19, J.W. Rice Jr.4, C. Schröder11, R.J. Sullivan1, A. Yen13, R.A. Yingst20 1 Dept. of Astronomy, Space Sciences Bldg., Cornell University, Ithaca, NY 14853, USA 2 Botanical Museum, Harvard University, Cambridge MA 02138, USA 3 Dept.
    [Show full text]
  • Mars Reconnaissance Orbiter and Opportunity Observations Of
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Mars Reconnaissance Orbiter and Opportunity 10.1002/2014JE004686 observations of the Burns formation: Crater Key Point: hopping at Meridiani Planum • Hydrated Mg and Ca sulfate Burns formation minerals mapped with MRO R. E. Arvidson1, J. F. Bell III2, J. G. Catalano1, B. C. Clark3, V. K. Fox1, R. Gellert4, J. P. Grotzinger5, and MER data E. A. Guinness1, K. E. Herkenhoff6, A. H. Knoll7, M. G. A. Lapotre5, S. M. McLennan8, D. W. Ming9, R. V. Morris9, S. L. Murchie10, K. E. Powell1, M. D. Smith11, S. W. Squyres12, M. J. Wolff3, and J. J. Wray13 1 2 Correspondence to: Department of Earth and Planetary Sciences, Washington University in Saint Louis, Missouri, USA, School of Earth and Space R. E. Arvidson, Exploration, Arizona State University, Tempe, Arizona, USA, 3Space Science Institute, Boulder, Colorado, USA, 4Department of [email protected] Physics, University of Guelph, Guelph, Ontario, Canada, 5Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 6U.S. Geological Survey, Astrogeology Science Center, Flagstaff, Arizona, USA, 7 8 Citation: Department of Organismic and Evolutionary Biology, Harvard University, Cambridge, Massachusetts, USA, Department Arvidson, R. E., et al. (2015), Mars of Geosciences, Stony Brook University, Stony Brook, New York, USA, 9NASA Johnson Space Center, Houston, Texas, USA, Reconnaissance Orbiter and Opportunity 10Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland, USA, 11NASA Goddard Space Flight Center, observations of the Burns formation: Greenbelt, Maryland, USA, 12Department of Astronomy, Cornell University, Ithaca, New York, USA, 13School of Earth and Crater hopping at Meridiani Planum, J.
    [Show full text]
  • FIELD STUDIES of CRATER GRADATION in GUSEV CRATER and MERIDIANI PLANUM USING the MARS EXPLORATION ROVERS. J. A. Grant1, M. P. Golombek2, A
    Role of Volatiles and Atmospheres on Martian Impact Craters 2005 3004.pdf FIELD STUDIES OF CRATER GRADATION IN GUSEV CRATER AND MERIDIANI PLANUM USING THE MARS EXPLORATION ROVERS. J. A. Grant1, M. P. Golombek2, A. F. C. Haldemann2, L. Crumpler3, R. Li4, W. A. Watters5, and the Athena Science Team 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, 2Jet Propulsion Laboratory, California Institute of Tech- nology, Pasadena, CA 91109, 3New Mexico Museum of Natural History and Science, Albuquerque, NM 87104, 4Department of Civil Engineering and Remote Sensing, The Ohio State University, Columbus, OH 43210, 5Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139. Introduction: The Mars Exploration Rovers Spirit Impact Structures in Meridiani Planum: Craters and Opportunity investigated numerous craters since explored at Meridiani are fewer and farther between landing in Gusev crater (14.569oS, 175.473oE) and than at Gusev and all are formed into sulfate bedrock Meridiani Planum (1.946oS, 354.473oE) over the first [3]. With the exception of the most degraded examples, 400 sols of their missions [1-4]. Craters at both sites Meridiani craters have depth-to-diameter ratios >0.10 are simple structures and vary in size and preservation and preserve walls sloped generally >10 degrees. En- state. Comparing observed and expected pristine mor- durance crater is 150 m-in-diameter, 22 m deep, and phology and using process-specific gradational signa- possesses walls sloped between 15-30 degrees, but tures around terrestrial craters as a template [5-7] al- locally exceeding the repose angle (Table 1).
    [Show full text]
  • Sedimentary Textures Formed by Aqueous Processes, Erebus Crater, Meridiani Planum, Mars
    Sedimentary textures formed by aqueous processes, Erebus crater, Meridiani Planum, Mars J. Grotzinger Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA J. Bell III Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, New York 14853, USA K. Herkenhoff United States Geological Survey, Flagstaff, Arizona 86001, USA J. Johnson A. Knoll Botanical Museum, Harvard University, Cambridge, Massachusetts 02138, USA E. McCartney Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, New York 14853, USA S. McLennan Department of Geosciences, State University of New York, Stony Brook, New York 11794-2100, USA J. Metz Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA J. Moore National Aeronautics and Space Administration Ames, Space Science Division, Moffett Field, California 94035, USA S. Squyres Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, New York 14853, USA R. Sullivan O. Ahronson Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA R. Arvidson Department of Earth and Planetary Sciences, Washington University, St. Louis, Missouri 63130, USA B. Joliff M. Golombek Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA K. Lewis Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125,
    [Show full text]
  • The Modification Stage of Basin Formation
    Schultz P. H. and Merrill R. B., eds. Multi-ring Basins, Proc. LIUlar Planet. Sci. (1981), 12A, p. W-257. Printed in U.S.A. 1981mrbf.conf..227C The modification stage of basin formation: Conditions of ring formation Steven Kent Croft Lunar and Planetary Institute, 3303 NASA Road 1, Houston, Texas 77058 Abstract-The sequence of crater and basin morphologies has been re-examined to establish a classification scheme of basin ring structural types. Rings were classified on the basis of morphology, morphometry, transitional basin types, characteristic geophysical signatures, theoretical scaling and collapse models, and structural analyses of terrestrial impacts. Simple and complex craters, central peak-, peak ring-, and multiring-basins form a single continuous morphological and structural sequence with no apparent discontinuities. New rings characteristically appear between the main rim and the next inner structure (ring or peak) initially as incomplete and inconspicuous structures that become more complete and prominent with increasing rim diameter. Incipient structures of central peaks and new rings apparently begin to form at basin diameters significantly smaller than the diameters at which they first become visually detectable. Of the six classifiable ring structures, Ridge rings and Peak rings form within the collapsed central uplift (the latter from competent rocks on the flanks of the central uplift), Intermediate and Secondary Intermediate rings originate in the Horst and Graben megablock zone, Main Outer rims are fault scarps forming at a constant radial position in the strength crater, and Outer rings may be associated with the strength crater boundary. All basin rings, with the possible exception of Outer rings, form within the strength crater.
    [Show full text]
  • Mars-Base-Camp-2028.Pdf
    Mars Base Camp An Architecture for Sending Humans to Mars by 2028 A Technical Paper Presented by: Timothy Cichan Stephen A. Bailey Lockheed Martin Space Deep Space Systems, Inc. [email protected] [email protected] Scott D. Norris Robert P. Chambers Lockheed Martin Space Lockheed Martin Space [email protected] [email protected] Robert P. Chambers Joshua W. Ehrlich Lockheed Martin Space Lockheed Martin Space [email protected] [email protected] October 2016 978-1-5090-1613-6/17/$31.00 ©2017 IEEE Abstract—Orion, the Multi-Purpose Crew Vehicle, near term Mars mission is compelling and feasible, is a key piece of the NASA human exploration and will highlight the required key systems. architecture for beyond earth orbit (BEO). Lockheed Martin was awarded the contracts for TABLE OF CONTENTS the design, development, test, and production for Orion up through the Exploration Mission 2 (EM- 1. INTRODUCTION ..................................................... 2 2). Additionally, Lockheed Martin is working on 2. ARCHITECTURE PURPOSE AND TENETS ....................... 3 defining the cis-lunar Proving Ground mission 3. MISSION CAMPAIGN, INCLUDING PROVING GROUND architecture, in partnership with NASA, and MISSIONS ................................................................ 5 exploring the definition of Mars missions as the 4. MISSION DESCRIPTION AND CONCEPT OF OPERATIONS . 7 horizon goal to provide input to the plans for 5. ELEMENT DESCRIPTIONS ....................................... 13 human exploration of the solar system. This paper 6. TRAJECTORY DESIGN ............................................ 16 describes an architecture to determine the 7. SCIENCE ............................................................. 19 feasibility of a Mars Base Camp architecture 8. MARS SURFACE ACCESS FOR CREW ......................... 14 within about a decade.
    [Show full text]
  • Endurance Crater at Meridiani Planum, Mars ⇑ Wesley A
    Icarus 211 (2011) 472–497 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Origin of the structure and planform of small impact craters in fractured targets: Endurance Crater at Meridiani Planum, Mars ⇑ Wesley A. Watters a, , John P. Grotzinger b, James Bell III a, John Grant c, Alex G. Hayes b, Rongxing Li d, Steven W. Squyres a, Maria T. Zuber e a Department of Astronomy, Cornell University, Ithaca, NY 14853, USA b Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 21125, USA c National Air and Space Museum, Smithsonian Institution, Washington, DC 20013, USA d Department of Civil and Environmental Engineering and Geodetic Science, Ohio State University, Columbus, OH 43210, USA e Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA article info abstract Article history: We present observations and models that together explain many hallmarks of the structure and growth Received 29 March 2010 of small impact craters forming in targets with aligned fractures. Endurance Crater at Meridiani Planum Revised 12 August 2010 on Mars (diameter 150 m) formed in horizontally-layered aeolian sandstones with a prominent set of Accepted 18 August 2010 wide, orthogonal joints. A structural model of Endurance Crater is assembled and used to estimate the Available online 19 September 2010 transient crater planform. The model is based on observations from the Mars Exploration Rover Oppor- tunity: (a) bedding plane orientations and layer thicknesses measured from stereo image pairs; (b) a dig- Keywords: ital elevation model of the whole crater at 0.3 m resolution; and (c) color image panoramas of the upper Impact processes crater walls.
    [Show full text]
  • Structural Analysis of Victoria Crater: Implications for Past Aqueous Processes on Mars
    Structural Analysis of Victoria Crater: Implications for Past Aqueous Processes on Mars By Serenity Mahoney A thesis submitted in partial fulfillment of the requirements of the degree of Bachelor of Arts (Geology) at Gustavus Adolphus College 2015 Structural Analysis of Victoria crater: Implications for Past Aqueous Processes on Mars By Serenity Mahoney Under the supervision of Dr. Julie Bartley ABSTRACT Visible across the surface of Mars, sedimentary structures are all that remains of the liquid water that once covered the planet. Despite their excellent exposure and wide extent, little is known about the exposed stratigraphy found in impact craters on Mars. With the next Mars rover mission scheduled for 2020, impact craters preserve multiple structural features formed both during impact and later during diagenesis, making them an ideal place to look for aqueous markers and therefore conditions suitable for ancient life. Analyses of exposed structural features in Victoria crater permits calculation of the orientation of these features and, combined with mineralogical evidence, provide definitive support for past regional aqueous processes. In this study, three images of the well-exposed promontory Cabo Anonimo in Victoria were analyzed using the program ImageRover. These analyses suggested evidence for multiple types of sedimentary bedding, including bedding within clasts in the crater wall and bedding within the wall itself. Bedding within the clasts suggests primary bedding pre-impact, possibly formed by aqueous processes. 2 ACKNOLEDGEMENTS I would like to thank my advisor Dr. Julie Bartley as well as Dr. Jim Welsh and Dr. Laura Triplett of the Geology department at Gustavus Adolphus College for their unwavering support and guidance.
    [Show full text]
  • Mars: Earth's Little Brother
    Mars: Earth’s little brother What are the similarities and differences you notice? Mars’s axis is tilted at 25 deg. What are seasons on Mars like? Mars’s axis tilt changes dramatically. What happens when the tilt is less/more? Artist’s depiction of an ‘icy Mars’ Do the Earth and Mars have similar interiors? Why? How do we even know what’s inside a planet? Atmospheres: Are they similar? Why? Constituents: Nitrogen: 78%! Carbon Doxide: 95.% Oxygen: 21 %! Nitrogen: 3%! Argon: 0.9%! Argon: 2%! Water: > 1%! Oxygen: 0.1%! Carbon Doxide: 0.002%! Water: > 0.03%! Is there water on Mars? Why or why not? Is there water on Mars? Why or why not? Mars’s south pole Is there water on Mars? Why or why not? Phase Diagram of Water Earth Partial Pressure of Water PartialPressure of Water Mars Temperature Is geology on Mars similar to that on Earth? Does this look like the Earth? What kind of geologic processes can you see evidence for? Notice any big impact craters? Olympus Mons: The biggest volcano in the solar system Olympus Mons: The biggest volcano in the solar system Is this similar to volcanoes on Earth? Valles Marineris: The solar system’s biggest canyon Our ‘grand’ canyon Mars or Earth? Mars or Earth? Columbia Hills, Mars Atacama Desert, Chile Columbia Hills, Mars Mars or Earth? Mars or Earth? Kilauea Volcanoe, Hawaii Olympus Mons, Mars Mars or Earth? Mars or Earth? Dubai, UAE Endurance Crater, Mars What is the evidence for past water on Mars? Mars or Earth? Mars or Earth? Djado Plateau, Niger Valles Marineris, Mars Mars or Earth? Mars or Earth? Holden Crater NE, Mars Lena Delta, Argentina Mars or Earth? Yemen Mars or Earth? Mars Mars or Earth? Mars or Earth? Niger Mars Seven minutes of terror Curiosity descent http://www.youtube.com/watch?v=gZX5GRPnd4U Google Mars Mars: Take-away messages •"Although smaller than Earth, Mars and Earth are similar in many ways.
    [Show full text]
  • Seeds and Supplies 2021
    FEDCO 2021 Seeds and Supplies Where Is erthing Ordering Instructions page 160 Order Forms pages 161-166 Complete Index inside back cover begin on page Welcome to Fedco’s rd ear Vegetable Seeds 5 “May you live in interesting times”… redux. Herb Seeds 79 How eerily prescient it was to invoke that adage a year Flower Seeds 86 ago—and then to experience it play out as both a curse and a blessing. Onion Sets & Plants 110 So much has shifted in a year. In our last catalog we Ginger, turmeric, sweet potato 111 brought you interviews with innovators in agriculture whose Potatoes 111 wisdom spoke to a more inclusive, regenerative and Farm Seed / Cover Crops 118 holistic future. Those visions, with all the excitement and challenge they bring, are rapidly taking hold and Soil Amendments 124 rooting in the disturbance of 2020. Pest Control 134 We see it all around us: my son’s cul-de-sac Tools 140 organized to grow food together. Neighborhoods Books 151 started seed banks. Signs sprang up in towns for Planting Guides & Lists: Give & Take tables for garden produce, to share what you can and take what you need. Winona La Duke, in Vegetable Chart 77 her (online) Common Ground Fair keynote, stressed the Botanical Index 78 building of local infrastructures. If we look outside the Herb Chart 79 strident newsfeed, we see new structures evolving from Flower Chart 86 common values. Seed Longevity Charts 92, 106 So in this year’s interviews we take a closer look at Organic Variety List 104 what’s unfolding.
    [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]