Conference on Early Mars, Geologic And

Total Page:16

File Type:pdf, Size:1020Kb

Conference on Early Mars, Geologic And CONFERENCE ON EARLY MARS: GEOLOGIC AND HYDROLOGIC EVOLUTION, PHYSICAL AND CHEMICAL ENVIRONMENTS, AND THE IMPLICATIONS FOR LIFE • • boiling :· • ·• hot springs ~- =· ',; ::,·,~~~ April24-27, 1997 Houston, Texas CONFERENCE ON EARLY MARS: GEOLOGIC AND HYDROLOGIC EVOLUTION, PHYSICAL AND CHEMICAL ENVIRONMENTS, AND THE IMPLICATIONS FOR LIFE Edited by S.M. Clifford, A. H. Treiman, H. E. Newsom, and J. D. Farmer Held at Houston, Texas April24-27, 1997 Sponsored by Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution Number 916 Compiled in 1997 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This report may be cited as Clifford S. M., Treiman A. H., Newsom H. E., and Farmer J. D., eds. (1997) Conference on Early .Mars: Geologic and Hydrologic Evolution, Physical and Chemical Environments, and the lmplicationsfor Life. LPI Contribution No. 916, Lunar and Planetary Institute, Houston. 87 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Mail order requestors will be invoiced for the cost of shipping and handling. "Each ofus is a tiny being, permitted to ride on the outermost skin ofone ofthe smaller planets for a few dozen trips around the local star ... We are fleeting, transitional creatures, snowflakes fallen on the hearth fire. That we understand even a little of our origins is one of the great triumphs of human insight and courage." -from Shadows of Forgotten Ancestors In Memory of Carl Sagan (1934-1996) Photo by Michael Okoniewski. Copyright © 1994. LPI Contribution No. 916 v Preface This volume contains abstracts that have been accepted for presentation at the Conference on Early Mars: Geologic and Hydrologic Evolution, Physical and Chemical Environments, and the Implications for Life, April 24-27, 1997, in Houston, Texas. The conveners for the conference were Stephen Clifford (Lunar and Planetary Institute), Allan Treiman (Lunar and Plan­ etary Institute), Horton Newsom (University ofNew Mexico), and Jack Fanner (NASA Ames Research Center). Members of the Scientific Organizing Committee included Michael Carr (U.S. Geological Survey), Benton Clark (Lockheed Martin), Roger Clark (U.S. Geological Survey), Michael Drake (University ofArizona), Fraser Fanale (University ofHawai 'i), Matthew Golombek (Jet Propulsion Labora­ tory), James Gooding (NASA Johnson Space Center), Virginia Gulick (NASA Ames Research Center), Bob Haberle (NASA Ames Research Center), Alan Howard (University of Virginia), Bruce Jakosky (University ofColorado), James Kasting (Pennsylvania State University), Ted Maxwell (National Air & Space Museum), George McGill (University ofMassachusetts), Christo­ pher McKay (NASA Ames Research Center), David McKay (NASA Johnson Space Center), Richard Morris (NASA Johnson Space Center), Susan Postawko (University of Oklahoma), Carl Sagan (Cornell University), Peter Schultz (Brown University), Everett Shock (Washington University), Steven Squyres (Cornell University), Carol Stoker (NASA Ames Research Center), and Kenneth Tanaka (U.S. Geological Survey). Logistics and administrative and publications support were provided by the Publications and Program Services Department staff at the Lunar and Planetary Institute. LPJ Contribution No. 916 vii Contents Mossbauer Spectroscopy of Thermal Springs Iron Deposits as Martian Analogs D. G. Agresti, T. J. Wdowiak, M. L. Wade, and L. P. Armendarez .................................................... 1 Geologic Alteration and Life in an Extreme Environment: Pu 'u Waiau, Mauna Kea, Hawai'i C. C. Allen, R. V Morris, D. C. Golden, and C. S. Upchurch ........................................................... 2 The Early Martian Climate Was Episodically Warm and Wet V R. Baker .......................................................................................................................................... 3 Developing a Chemical Code to Identify Magnetic Biominerals (Biomagnetite and Biogreigite) in Mars Soil and Rocks A. Ban in and R. L. Mancinelli ............................................................................................................ 4 Effect of Impacts on Early Martian Geologic Evolution N G. Barlow ....................................................................................................................................... 5 Biomarkers for Analysis of Martian Samples L. Becker, G. D. McDonald, and J. L. Bada ...................................................................................... 6 Application of the CHEMIN XRDIXRF Instrument in Analyzing Diagnostic Mineralogies: Quantitative XRD Analysis of Aragonite and Basalt D. Bish, D. Vaniman, P. Sarrazin, D. Blake, S. Chipera, S. A. Collins, and T. Elliott ....................................................................................................................................... 8 Spectroscopic Identification of Minerals in Hematite-bearing Soils and Sediments: Implications for Chemistry and Mineralogy of the Martian Surface J. L. Bishop, J. Friedl, and U. Schwertmann ...................................................................................... 9 39 Ar_4o Ar Age of Allan Hills 84001 D. D. Bogard and D. H Garrison.................................................................................................... 10 Scientific Issues Addressed by the Mars Surveyor 2001 Gamma-Ray/Neutron Spectrometer (GRS/NS) W. V Boynton, W. C. Feldman, S. W. Squyres, J.l. Trombka, J. R. Arnold, P. A. J. Englert, A. E. Metzger, R. C. Reedy, H Wanke, S. H. Bailey, J. Briickner, L. G. Evans, H Y. McSween, and R. Starr .................................................................. 12 Experimental Studies ofMars-Analog Brines M A. Bullock, J. M Moore, and M T. Mellon ................................................................................ 13 Hydrogeology and Exobiology Significance of Martian Large Crater Lakes N. A. Cabrol and E. A. Grin .. .. ... ............ ... ... .. .. .. .. .......... ........ .... .. .. ... ............ ... ... .. ... .. ... .. 14 viii Conference on Early Mars Microbial Diversity in Hyperthermophilic Biofilms: Implications for Recognizing Biogenicity in Hydrothermal Deposits S. L. Cady, C. E. Blank, D. J. Des Marais, M. R. Walter, and J.D. Farmer ................................... 15 The Highlands Crust of Mars and the Pathfinder Mission: A Prospective View from Mariner 6 Infrared Spectroscopy W. M. Calvin, A. H. Treiman, and L. Kirkland ................................................................................. 16 Thermal Loss ofWater on Young Planets: The Effect of a Strong Primitive Solar Wind E. Chasseftere...................... ... .. .. .. .. .. .. .. .. .. .. ... .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ... .. .. .. 17 Geochemical Cycles of CHNOPS and Other Potentially Important Biological Elements on Mars B. C. Clark ........................................................................................................................................ 18 Hydraulic and Thermal Constraints on the Development of the Martian Valley Networks S. M Cliff'ord . .. ... .. .. .. .. .. ... ... ... .. .. .. .. .. .. .. .. .. ... .. .. .. .. .. .. .. .. .. .. .. ... .. .. .. .. .. .. .. .. ... .. 18 The Origin of the Martian Intercrater Plains: The Role of Liquefaction from Impact and Tectonic-induced Seismicity S. M Cliff'ord .. .. .. .. .. .. .. ... .. .. .. .. .. .. .. .. .. .. .. .. .. .. .... .. .. ... .. ... .. .. .. .. .. .. .. .. .. .. .. .. .. 19 The Early History of Mars as Told by Degraded Highland Impact Craters R. A. Craddock, T. A. Maxwell, and A. D. Howard ......................................................................... 20 The Radiative Effects of C02 Ice Clouds on the Early Martian Climate D. Crisp and R. T. Pierrehumbert .................................................................................................... 21 Degradation of the Martian Cratered Highlands: The Role ofCircum-Hellas Outflow Channels and Constraints on the Timing of Volatile-driven Activity D. A. Crown, S. C. Mest, and K. H Stewart ..................................................................................... 22 Mars on Earth: Antarctic Dry Valley Lakes and Their Deposits P. T. Doran and R. A. Wharton ........................................................................................................ 24 Accretion of Earth and Mars: Implications for Bulk Composition and Volatile Inventories M J. Drake ....................................................................................................................................... 24 Volatile Inventories of Mars and Earth and Their Implication for the Evolution of Planetary Atmospheres G. Dreibus, H Wanke, and G. W. Lugmair ..................................................................................... 26 LPI Contribution No. 916 ix Regarding a Wet, Early Noachian Mars: Geomorphology of Western Arabia and Northern Sinus Meridiani K. S. Edgett and T. J. Parker
Recommended publications
  • Planetary Geologic Mappers Annual Meeting
    Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m.
    [Show full text]
  • Thermal Studies of Martian Channels and Valleys Using Termoskan Data
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 99, NO. El, PAGES 1983-1996, JANUARY 25, 1994 Thermal studiesof Martian channelsand valleys using Termoskan data BruceH. Betts andBruce C. Murray Divisionof Geologicaland PlanetarySciences, California Institute of Technology,Pasadena The Tennoskaninstrument on boardthe Phobos '88 spacecraftacquired the highestspatial resolution thermal infraredemission data ever obtained for Mars. Included in thethermal images are 2 km/pixel,midday observations of severalmajor channel and valley systems including significant portions of Shalbatana,Ravi, A1-Qahira,and Ma'adimValles, the channelconnecting Vailes Marineris with HydraotesChaos, and channelmaterial in Eos Chasma.Tennoskan also observed small portions of thesouthern beginnings of Simud,Tiu, andAres Vailes and somechannel material in GangisChasma. Simultaneousbroadband visible reflectance data were obtainedfor all but Ma'adimVallis. We find thatmost of the channelsand valleys have higher thermal inertias than their surroundings,consistent with previousthermal studies. We show for the first time that the thermal inertia boundariesclosely match flat channelfloor boundaries.Also, butteswithin channelshave inertiassimilar to the plainssurrounding the channels,suggesting the buttesare remnants of a contiguousplains surface. Lower bounds ontypical channel thermal inertias range from 8.4 to 12.5(10 -3 cal cm-2 s-1/2 K-I) (352to 523 in SI unitsof J m-2 s-l/2K-l). Lowerbounds on inertia differences with the surrounding heavily cratered plains range from 1.1 to 3.5 (46 to 147 sr). Atmosphericand geometriceffects are not sufficientto causethe observedchannel inertia enhancements.We favornonaeolian explanations of the overall channel inertia enhancements based primarily upon the channelfloors' thermal homogeneity and the strongcorrelation of thermalboundaries with floor boundaries. However,localized, dark regions within some channels are likely aeolian in natureas reported previously.
    [Show full text]
  • Seasonality and Surface Properties of Slope Streaks
    51st Lunar and Planetary Science Conference (2020) 2556.pdf SEASONALITY AND SURFACE PROPERTIES OF SLOPE STREAKS. K. M. Primm, R. H. Hoover, H. H. Kaplan, and D. E. Stillman, Dept. of Space Studies, Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302, USA ([email protected]). Background: Slope streaks are large (up to 200 m Methods: We used images from the High wide, up to a few km long), relatively low-albedo Resolution Imagining Science Experiment (HiRISE) to streaks that occur in the dustiest locations on Mars [1]. study the fading rate of slope streaks, Context Camera They are one of the few currently active and (CTX) to create Digital Terrain Models (DTMs) to widespread geologic processes on the surface of Mars. study the slope angles, and lastly the Compact Many slope streaks have persisted for >15 Mars years Reconnaissance Imaging Spectrometer (CRISM) to and others have been observed to form, but many evaluate the mineralogy of slope streaks and the fewer have been seen to completely fade/disappear surrounding terrain. (e.g., [2]). This inconsistency leads us to believe Results: Preliminary observations show that hypothesize that slope streaks might have different within one area (within a few kms), there are slope formation and fading mechanisms depending on their streaks that completely fade within 1 Mars Year and environment. some that form within that same time frame (Fig. 1). There have been several studies of slope streaks The green circles in Fig. 1B shows the newly formed that examine a combination of parameters: slope angles [1,3], mineralogy [4-6], environmental factors, slope streaks and the red circle show the areas where and seasonality [2,7,8] but none have combined all the slope streaks have completely disappeared.
    [Show full text]
  • No Change in the Recent Lunar Impact Flux Required Based On
    Geophysical Research Letters RESEARCH LETTER No Change in the Recent Lunar Impact Flux Required Based 10.1029/2018GL077254 on Modeling of Impact Glass Spherule Age Distributions Key Points: • An excess of young lunar impact glass Ya-Huei Huang1 , David A. Minton1, Nicolle E. B. Zellner2 , Masatoshi Hirabayashi3 , spherules <500 Ma likely results from 4 5 limited sampling depths where lunar James E. Richardson , and Caleb I. Fassett soils were collected • Sampling biases can explain the 1Department of Earth, Atmospheric, and Planetary Science, Purdue University, West Lafayette, IN, USA, 2Department of excess of young spherules, rather than Physics, Albion College, Albion, MI, USA, 3Department of Aerospace Engineering, Auburn University, Auburn, AL, USA, a significant change in the impact flux 4Planetary Science Institute, Tucson, AZ, USA, 5NASA Marshall Space Flight Center, Huntsville, AL, USA in the last 500 Ma • Using lunar impact glass spherule ages to constrain the impact flux may 40 39 be less biased if collected beyond the Abstract The distributions of Ar/ Ar-derived ages of impact glass spherules in lunar regolith uppermost lunar surface samples show an excess at <500 Ma relative to older ages. It has not been well understood whether this excess of young ages reflects an increase in the recent lunar impact flux or is due to a bias in the samples. Supporting Information: We developed a model to simulate the production, transport, destruction, and sampling of lunar glass • Supporting Information S1 spherules. A modeled bias is seen when either (1) the simulated sampling depth is 10 cm, consistent with the typical depth from which Apollo soil samples were taken, or (2) when glass occurrence in the ejecta is > Correspondence to: limited to 10 crater radii from the crater, consistent with terrestrial microtektite observations.
    [Show full text]
  • ROSS T. SHINYAMA #8830-0 SUMMER II. Kaiawtr I+9599-O First L-Lawaiian Center 999 Bishop Street, 23Rd Floor
    WATANABI] ING I-LP A Limited Liability [,aw Parrnership ":r : , 1 I ' I J. DOUGLAS ING #1538-0 i.,,i l i t I i '.tì ROSS T. SHINYAMA #8830-0 SUMMER II. KAIAWtr I+9599-O First l-lawaiian Center 999 Bishop Street, 23rd Floor Honolulu, Ilawaii 968 1 3 Telephone No.: (808) 544-8300 Facsimile No.: (808) 544-8399 E-mails : [email protected] Attorneys for TMT INTBRNATIONAL OBSBRVATORY, I,LC BOARD OF LAND AND NATURAL RESOURCES FOR THE STATE OF I]AWAI'I IN THE MATTER OF Case No. BLNR-CC -16-002 TMT INTERNATIONAL A Contested Case l{earing Re Conservation OBSBRVATORY, LLC'S PRE-HEARING District Use Permit (CDUP) I{A-3568 for the STATEMENT; EXHIBIT ..1,'; Thirty Meter Telescope at the Mauna Kea CERTIFICATE OF SERVICE Science Reserve, I(a'ohe Mauka, Hãmakua District, Island of Hawai'i, TMK (3) 4-4- 0l 5:009 TABLtr OF CONTBNTS IN'IRODUC]'ION II DI]SCRIPI'ION OF THE PROJECT AND ITS PROCI]DURAL HISTORY A. Description ofthe Project.................. 3 B. Procedulal Llistory 3 l. General Lease and the MI(SR 3 2. T'he Project 5 III. BURDEN OF PROOF I IV. ISSUES TO BE DECIDED AND TIO'S STATEMENT OF POSI'|iON.. A. The Project, Including the Plans Incorporatcd in the Application, is Consistent with Chapter 183C of the Hawai'i Revised Statutes, the Criteria in HAR $ 13-5- 30(c), and Other Applicable Conservation District Rules......... ..........9 i. The Project is consistent with the purpose of the Conservation District.. 10 2. The Project is consistent with the objectives of the sub2one...................
    [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]
  • DATING the RESURFACING EVENTS of the HARMAKHIS VALLIS SOURCE REGIONS, MARS: PRELIMINARY RESULTS. S. Kukkonen and V.-P
    44th Lunar and Planetary Science Conference (2013) 2140.pdf DATING THE RESURFACING EVENTS OF THE HARMAKHIS VALLIS SOURCE REGIONS, MARS: PRELIMINARY RESULTS. S. Kukkonen and V.-P. Kostama, Astronomy, Department of Physics, P.O. Box 3000, FI-90014 University of Oulu, Finland ([email protected]). Introduction: Harmakhis Vallis is one of the four [e.g., 15–17]. Usually they have been excluded from major outflow channel systems that cut the eastern Hel- the crater counts because of the uncertainty of their las rim region of Mars (Fig. 1). It is ~800 km long and origin (primary vs. secondary crater). However, small located ~450 km south of Hadriaca Patera starting craters accumulate to the surface more quickly than close to the end of another valley, Reull Vallis. Due to larger ones, and thus the high spatial resolution is nec- the close position to the volcanic features, the channels essary in dating younger surfaces or small units where are suggested to have been formed by the mobilization there are only few large craters. In the case of Harma- and release of subsurface volatiles by volcanic heat [1– khis Vallis, the region has experienced significant re- 5]. Because Harmakhis Vallis cuts the surrounding cent modification and degradation, and thus, we can massifs of the cratered terrains, it is clearly one of the assume that the small crater population mostly post- youngest features in the region [6, 7]. dates the secondary craters forming larger impacts lo- cated in the older regions. Therefore, only the obvious clusters of secondary craters were excluded from the counts.
    [Show full text]
  • NITROGEN on MARS: INSIGHTS from CURIOSITY. J. C. Stern1 , B. Sutter2, W. A. Jackson3, Rafael Na- Varro-González4, Christopher P
    Lunar and Planetary Science XLVIII (2017) 2726.pdf 1 2 3 NITROGEN ON MARS: INSIGHTS FROM CURIOSITY. J. C. Stern , B. Sutter , W. A. Jackson , Rafael Na- varro-González4, Christopher P. McKay5, Douglas W. Ming6, P. Douglas Archer2, D. P. Glavin1, A. G. Fairen7,8 and Paul R. Mahaffy1. 1NASA GSFC, Code 699, Greenbelt, MD 20771, [email protected], 2Jacobs, NASA Johnson Space Center, Houston, TX 77058, 3Texas Tech University, Lubbock, TX 79409, 4Universidad Nacional Autónoma de México, México, D.F. 04510, Mexico, 5NASA Ames Research Center, Moffett Field, CA 94035, 6NASA Johnson Space Center, Houston TX 77058, 7Centro de Astrobiologia, Madrid, Spain, 8Cornell University, Ithaca, NY 14853 Introduction: Recent detection of nitrate on Mars [1] indicates that nitrogen fixation processes occurred in early martian history. Data collected by the Sample Analysis at Mars (SAM) instrument on the Curiosity Rover can be integrated with Mars analog work in order to better understand the fixation and mobility of nitrogen on Mars, and thus its availability to putative biology. In particular, the relationship between nitrate and other soluble salts may help reveal the timing of nitrogen fixation and post-depositional behavior of nitrate on Mars. In addition, in situ measurements of nitrogen abundance and isotopic composition may be used to model atmospheric conditions on early Mars. Methods: The data presented are from analyses of solid Martian drilled and scooped samples by the Sam- ple Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) Curiosity Rover. SAM performs evolved gas analysis (EGA), in which a 3 Figure 1.
    [Show full text]
  • The 1997 Mars Pathfinder Spacecraft Landing Site: Spillover Deposits
    www.nature.com/scientificreports OPEN The 1997 Mars Pathfnder Spacecraft Landing Site: Spillover Deposits from an Early Mars Inland Sea Received: 13 June 2018 J. A. P. Rodriguez1, V. R. Baker2, T. Liu 2, M. Zarroca3, B. Travis1, T. Hui2, G. Komatsu 4, Accepted: 22 January 2019 D. C. Berman1, R. Linares3, M. V. Sykes1, M. E. Banks1,5 & J. S. Kargel1 Published: xx xx xxxx The Martian outfow channels comprise some of the largest known channels in the Solar System. Remote-sensing investigations indicate that cataclysmic foods likely excavated the channels ~3.4 Ga. Previous studies show that, in the southern circum-Chryse region, their fooding pathways include hundreds of kilometers of channel foors with upward gradients. However, the impact of the reversed channel-foor topography on the cataclysmic foods remains uncertain. Here, we show that these channel foors occur within a vast basin, which separates the downstream reaches of numerous outfow channels from the northern plains. Consequently, foods propagating through these channels must have ponded, producing an inland sea, before reaching the northern plains as enormous spillover discharges. The resulting paleohydrological reconstruction reinterprets the 1997 Pathfnder landing site as part of a marine spillway, which connected the inland sea to a hypothesized northern plains ocean. Our food simulation shows that the presence of the sea would have permitted the propagation of low-depth foods beyond the areas of reversed channel-foor topography. These results explain the formation at the landing site of possible fuvial features indicative of fow depths at least an order of magnitude lower than those apparent from the analyses of orbital remote-sensing observations.
    [Show full text]
  • GLOBAL HISTORY of WATER and CLIMATE. M. H. Carr, U.S. Geological Survey, 345 Middlefield Road, Menlo Park CA 94025, USA ([email protected])
    Fifth International Conference on Mars 6030.pdf GLOBAL HISTORY OF WATER AND CLIMATE. M. H. Carr, U.S. Geological Survey, 345 Middlefield Road, Menlo Park CA 94025, USA ([email protected]). Introduction: Despite acquisition of superb new ages.(05803,08205, 51304). In addition, areas that altimetry and imagery by Mars Global Surveyor, most appear densely dissected in Viking images commonly aspects of the water and climate story are likely to have poorly organized drainage patterns when viewed remain controversial. The relative roles of surface at the MOC scale (04304, 08905, 09306). Through- runoff and groundwater seepage in the formation of going valleys and an ordered set of tributaries are dif- valley networks are yet to be resolved as are the cli- ficult to discern. These areas more resemble terrestrial matic conditions required for their formation. Simi- thermokarst terrains than areas where fluvial proc- larly, the fate of the floodwaters involved in formation esses dominate. A few areas do, have more typical of the outflow channels remains unresolved. While the fluvial erosion patterns. At 26S, 84W numerous MOC images provide little supporting evidence for closely spaced tributaries feed larger valleys to form a proposed shorelines around an extensive global ocean dense, well integrated valley system (07705). Such [1], the altimetry suggests the presence of a bench at examples, are however, rare. constant altitude around the lowest parts of the north- Debates about the origin of valley networks have ern plains [2]. Here I describe some of the attributes of focused mainly on (1) the role of fluvial erosion versus the channels and valleys as seen in the early MOC other processes, (2) the relative roles of groundwaer images, summarize the evidence for climate change sapping and surface runoff, and (3) the climatic con- on Mars, and discuss some processes that might have ditions required for valley formation.
    [Show full text]
  • “Mining” Water Ice on Mars an Assessment of ISRU Options in Support of Future Human Missions
    National Aeronautics and Space Administration “Mining” Water Ice on Mars An Assessment of ISRU Options in Support of Future Human Missions Stephen Hoffman, Alida Andrews, Kevin Watts July 2016 Agenda • Introduction • What kind of water ice are we talking about • Options for accessing the water ice • Drilling Options • “Mining” Options • EMC scenario and requirements • Recommendations and future work Acknowledgement • The authors of this report learned much during the process of researching the technologies and operations associated with drilling into icy deposits and extract water from those deposits. We would like to acknowledge the support and advice provided by the following individuals and their organizations: – Brian Glass, PhD, NASA Ames Research Center – Robert Haehnel, PhD, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory – Patrick Haggerty, National Science Foundation/Geosciences/Polar Programs – Jennifer Mercer, PhD, National Science Foundation/Geosciences/Polar Programs – Frank Rack, PhD, University of Nebraska-Lincoln – Jason Weale, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory Mining Water Ice on Mars INTRODUCTION Background • Addendum to M-WIP study, addressing one of the areas not fully covered in this report: accessing and mining water ice if it is present in certain glacier-like forms – The M-WIP report is available at http://mepag.nasa.gov/reports.cfm • The First Landing Site/Exploration Zone Workshop for Human Missions to Mars (October 2015) set the target
    [Show full text]
  • Non-Collider Searches for Stable Massive Particles
    Non-collider searches for stable massive particles S. Burdina, M. Fairbairnb, P. Mermodc,, D. Milsteadd, J. Pinfolde, T. Sloanf, W. Taylorg aDepartment of Physics, University of Liverpool, Liverpool L69 7ZE, UK bDepartment of Physics, King's College London, London WC2R 2LS, UK cParticle Physics department, University of Geneva, 1211 Geneva 4, Switzerland dDepartment of Physics, Stockholm University, 106 91 Stockholm, Sweden ePhysics Department, University of Alberta, Edmonton, Alberta, Canada T6G 0V1 fDepartment of Physics, Lancaster University, Lancaster LA1 4YB, UK gDepartment of Physics and Astronomy, York University, Toronto, ON, Canada M3J 1P3 Abstract The theoretical motivation for exotic stable massive particles (SMPs) and the results of SMP searches at non-collider facilities are reviewed. SMPs are defined such that they would be suffi- ciently long-lived so as to still exist in the cosmos either as Big Bang relics or secondary collision products, and sufficiently massive such that they are typically beyond the reach of any conceiv- able accelerator-based experiment. The discovery of SMPs would address a number of important questions in modern physics, such as the origin and composition of dark matter and the unifi- cation of the fundamental forces. This review outlines the scenarios predicting SMPs and the techniques used at non-collider experiments to look for SMPs in cosmic rays and bound in mat- ter. The limits so far obtained on the fluxes and matter densities of SMPs which possess various detection-relevant properties such as electric and magnetic charge are given. Contents 1 Introduction 4 2 Theory and cosmology of various kinds of SMPs 4 2.1 New particle states (elementary or composite) .
    [Show full text]