DOCSLIB.ORG

Latitude of Landing Site

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Latitude of Landing Site Mars Landing Sites: Where would you go? Debra Buczkowski, Kim Seelos, and Wes Patterson NASA’s Mars Exploration Program Strategy: Follow the water, assess habitability, return a sample, prepare for humans MSL launch has been delayed to at least 2011 2 Types of Mars Missions . Orbital Missions . Instruments stay in orbit around Mars . Missions include: . Mariner, Viking Orbiters, Mars Global Surveyor (MGS), Mars Odyssey, Mars Reconnaissance Orbiter (MRO) . Surface Missions . Instruments on lander or rover . Missions include: . Viking Landers (1 and 2) . Mars Pathfinder (rover) . Mars Exploration Rovers . MER- A Spirit . MER-B Opportunity . Phoenix (lander) 3 Locations of successful landed missions Phoenix Viking 2 Viking 1 Pathfinder MER B MER A Opportunity Spirit 4 Guiding Principles . Landing site selection is critical to all aspects of mission and program success . No landing, no science . Final site recommendation, selection, and approval is the job of the Project, Science Team, and NASA headquarters . The broad expertise of the science community is crucial to the identification of optimal sites . Process can be open to all and has no predetermined outcome 5 Basis for Site Selection . Landing Sites Must Meet All Engineering Requirements . Engineering requirements can include: . Latitude of landing site . Elevation of landing site . Size of landing ellipse . Slope of landing site surface . Rock abundance at the landing site . Wind speed at the landing site 6 Engineering Requirements . Latitude . The latitude of a landing site is generally constrained by the lander’s energy source or science goals . Some missions have a power constraint . Solar powered landers need more direct sunlight . MER was constrained to a latitude band of 10°N to15°S . MSL has a wide latitude band of ±60° because it is not solar powered . Phoenix was designed for polar science . latitude band was 65-72°N 7 Engineering Requirements . Elevation . The elevation restrictions of a landing site depend upon the method of landing . Parachute landings require low elevations so that there is more atmosphere to reduce velocity . MSL can land at elevations up to +2.0 km . Provides access to ~83% of Mars . Includes most of the highlands . VL1, 2 & MPF had to land below <-3 km . Only options are in the Northern Lowlands . MER landing site elevations had to be <-1.3 km 8 MSL Landing Site Access Maps show -90º to 90º latitude; 180º to -180º W longitude; horizontal lines at 60º latitude; blacked out areas are > 2km elevation 9 Engineering Requirements . Rock abundance . The size and quantity of rocks at a landing site is very important to quantify Viking 2 landing site . Could damage the lander/rover upon landing Rejected Phoenix landing site 10 Engineering Requirements . Slope . Landing site can not be too steep or else the lander/rover will not be able to land safely . Wind Speed . Some regions of Mars are extremely windy . High winds could push the lander/rover into an unsafe area during landing . Unsafe areas could include cliffs, craters, extremely rocky regions, etc. 11 Engineering Requirements . Landing Ellipse Size . The ideal landing site, plus an allowance for error, defines the landing ellipse . Size of the landing ellipse depends upon the landing method, e.g., . Parachute w/ airbag . Reverse thrusters Artist rendering of airbag system used for the MERs . Sky crane . Goal is to land in the center of the ellipse but any other area within the ellipse needs to be safe . Low slope . Smooth . Not too windy Artist rendering of sky crane for MSL 12 Engineering Requirements . Ellipse Size . Number of possible landing sites scales with ellipse size . Beagle (Length 500 km = 1 Site) . MPF (Length 200-300 km = <10 Sites) . MER (Length ~100 km = ~150 Sites) . MSL has a small ~20 km diameter ellipse . Allows 103 to 109 potential sites plus “Go To” ability . Can traverse out of the landing ellipse to any area of interest . Future Missions Could Have Different Constraints…. MER-A Spirit Landing Ellipse 13 Basis for Site Selection . Potential Landing Sites Must Also Meet Science Requirements . To determine if a site meets the science requirements we must be able to: . Characterize the geology of the region of interest . Assess the relative age compared to other regions of the planet . Assess biological potential . Morphology consistent with water-related activity . Geochemistry/mineralogy . Characterize climate history at region of interest . The role of water . Surface/atmosphere interaction 14 Example of water related geomorphology .A color-enhanced image of the delta in Jezero Crater .Once held a lake .Ancient rivers ferried minerals into the lake .Clay-like minerals are shown in green .Form the delta .Clays tend to trap and preserve organic matter .Delta thus a good place to look for signs of ancient life on Mars Image credit: NASA/JPL/JHUAPL/MSSS/Brown University. 15 Basis for Site Selection . Engineering and science constraints are mapped into potential landing sites on Mars . Use available remote sensing data . New orbital data of can be acquired . MSL sites have priority in the scheduling of MRO targets . All potential landing sites must be defendable . Must survive multiple reviews, so be thorough . Do everything to understand surface properties . Factor mission science objectives into selection . Selection must be done openly . Multiple opportunities for community involvement . Open workshops . Provide science community input to landing site . Also educational opportunities & public outreach 16 Planetary Protection Requirements . There is a Planetary Protection Office . Landing sites must comply with guidelines . Must not have known water or water-ice within one meter of the surface . Some regions are special exceptions . Purpose of the Phoenix mission was to sample water ice . It had to be allowed to land in a water-rich area Phoenix robotic arm in lab . Robotic arm was sterilized and wrapped in bio-barrier . There are areas interpreted to have a high potential for the existence of native martian life forms . Missions looking for life would have to be allowed to land there Phoenix arm bio-barrier . Unfortunately, this also where terrestrial organisms are likely to propagate 17 MSL Rover Overview Conceptual Design 18 MSL compared with MER Conceptual Design 19 Summary of Current Engineering Constraints on MSL Landing Sites 20 Scientific Objective of MSL . Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present 21 Scientific Objective of MSL • Assessment of present habitability requires: . An evaluation of the characteristics of the environment and the processes that influence it from microscopic to regional scales . A comparison of these characteristics with what is known about the capacity of life, as we know it, to exist in such environments . Assessment of past habitability also requires inferring environments and processes in the past from observation in the present . Requires integration of a wide variety of chemical, physical, and geological measurements and analyses 22 Scientific Objectives for MSL Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present. Assess the biological potential of at least one target environment. Determine the nature and inventory of organic carbon compounds . Inventory the chemical building blocks of life (C, H, N, O, P, S) . Identify features that may represent the effects of biological processes 23 Scientific Objectives for MSL Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present. Characterize the geology and geochemistry of the landing region at all appropriate spatial scales (i.e., ranging from micrometers to kilometers) . Investigate the chemical, isotopic, and mineralogical composition of martian surface and near-surface geological materials . Interpret the processes that have formed and modified rocks and regolith 24 Scientific Objectives for MSL Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present. Investigate planetary processes of relevance to past habitability, including the role of water . Assess long-timescale (i.e., 4-billion-year) atmospheric evolution processes . Determine present state, distribution, and cycling of water and CO2 25 Scientific Objectives for MSL Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present. Characterize the broad spectrum of surface radiation, . Galactic cosmic radiation . Solar proton events . Secondary neutrons 26 Scientific Investigations Overview Remote Sensing MastCam imaging, atmospheric opacity ChemCam chemical composition, imaging Contact APXS chemical composition MAHLI microscopic imaging Analytic Laboratory SAM chemical and isotopic composition, including organic molecules CheMin mineralogy, chemical composition Environmental DAN subsurface hydrogen MARDI landing site descent imaging REMS meteorology / UV radiation RAD high-energy radiation Total 10 • MSL also carries a sophisticated sample acquisition, processing and handling system. • >120 investigators and collaborators. • Significant international participation: Spain, Russia, Germany, Canada, France, Finland. 27 Summary: Investigations vs. Objectives Mast- Chem- Che- MAHLI APXS SAM MARDI DAN REMS RAD Objective: Cam Cam Min Determine the nature and inventory of + ++ + organic carbon compounds. Inventory the chemical building
Load more

Recommended publications
  • A Step Toward Mars University of Dayton
    University of Dayton eCommons News Releases Marketing and Communications 4-26-2017 A Step Toward Mars University of Dayton Follow this and additional works at: https://ecommons.udayton.edu/news_rls Recommended Citation University of Dayton, "A Step Toward Mars" (2017). News Releases. 10986. https://ecommons.udayton.edu/news_rls/10986 This News Article is brought to you for free and open access by the Marketing and Communications at eCommons. It has been accepted for inclusion in News Releases by an authorized administrator of eCommons. For more information, please contact [email protected], [email protected]. Wednesday April 26, 2017 R E L A T E D A STEp TOWARD MARS A R T I C L E S A highly successful test of a prototype power generator Come on at the University of Dayton Research Institute bodes well for NASA's plans to expand its exploration of Mars over Mars with the next rover mission. Rover In early February, NASA scientists narrowed down potential landing sites for Mars 2020 to three — Northeast Syrtis, Jezero Crater and Columbia Hills — at least one of which is likely to be warmer than sites where previous rovers landed. Simultaneously, researchers in Dayton performed a high-temperature qualifying test on a power generator prototype to see if it would operate successfully at the higher temperatures that may be experienced by the generator powering the next rover. The Mars 2020 rover will be powered by a Multi-Mission Radioisotope Thermoelectric Generator (MMRTG) — similar to the unit currently providing power to Curiosity in Gale Crater — which converts heat created by naturally decaying plutonium radioisotopes into electricity to power the rover's instruments, computers, wheels, robotic arm and radio.
    [Show full text]
  • Hip # 987-1088
    Hip No. Consigned by Tate Farms Hip No. 987 Jess Sizzlin SI 92 987 1997 Sorrel Mare Streakin La Jolla SI 99 {Streakin Six SI 104 Mr Jess Perry SI 113 { Bottom’s Up SI 82 Scoopie Fein SI 99 {Sinn Fein SI 98 Jess Sizzlin SI 92 Legs La Scoop SI 95 3654393 Easy Jet SI 100 {Jet Deck SI 100 Sizzlin Kim SI 86 Lena’s Bar TB SI 95 (1987) { Sun Spots {Double Bid SI 100 Winsum Miss SI 95 By MR JESS PERRY SI 113 (1992). Champion 2-year-old, $687,184 [G1]. Sire of 799 ROM, 107 stakes winners, $39,619,142, incl. champions APOL- LITICAL JESS SI 107 (world champion, $1,399,831, Los Alamitos Derby [G1]), ONE FAMOUS EAGLE SI 101 ($1,387,453 [G1]). Sire of the dams of 46 stakes winners, incl. BODACIOUS DASH SI 101 ($756,495 [G1]), JES A GAME SI 111 ($323,978 [G2]), TERRIFIC SYNERGY SI 92 ($288,066 [RG2]). 1st dam SIZZLIN KIM SI 86, by Easy Jet. Placed to 3. Dam of 7 foals, 6 to race, 3 winners, including– Jess Sizzlin SI 92 (f. by Mr Jess Perry). Stakes placed winner, below. Streakin Kim (f. by Streakin La Jolla). Unplaced. Dam of– Kims Corona SI 97 (g. by Corona Cocktail). 3 wins to 4, $38,666. 2nd dam SUN SPOTS, by Double Bid. Unraced. Dam of 13 starters, 7 ROM, incl.– SUN KISSES SI 102 (f. by Game Plan). 7 wins to 3, $68,935, Shebester Derby, Mystery Derby. Dam of Exquisite Expense SI 99 ($42,264 [G3]).
    [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]
  • The Deposition and Alteration History of the Northeast Syrtis Major Layered Sulfates
    The deposition and alteration history of the northeast Syrtis Major layered sulfates Daven P. Quinn1 and B.L. Ehlmann1,2 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA October 12, 2018 Abstract The ancient stratigraphy on the western margin of the Isidis basin records the history of wateron early Mars. Noachian units are overlain by layered, basaltic-composition sedimentary rocks that are enriched in polyhydrated sulfates and capped by more resistant units. The layered sulfates – uniquely exposed at northeast Syrtis Major – comprise a sedimentary sequence up to 600-m thick that has undergone a multi-stage history of deposition, alteration, and erosion. Siliciclastic sed- iments enriched in polyhydrated sulfates are bedded at m-scale and were deposited on slopes up to 10°, embaying and thinning against pre-existing Noachian highlands around the Isidis basin rim. The layered sulfates were then modified by volume-loss fracturing during diagenesis, and the fractures hosted channelized flow and jarosite mineral precipitation to form resistant ridges upon erosion. The depositional form and diagenetic volume-loss recorded by the layered sulfates suggest deposition in a deepwater basin. After their formation, the layered sulfates were first capped by a “smooth capping unit” and then eroded to form paleovalleys. Hesperian Syrtis Ma- jor lavas were channelized by this paleotopography, capping it in some places and filling it in others. Later fluvial features and phyllosilicate-bearing lacustrine deposits, which share a con- sistent regional base level (~-2300 m), were superimposed on the sulfate-lava stratigraphy.
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • Towards Bioinspired in Vitro Models of Intestinal Mucus
    RSC Advances REVIEW View Article Online View Journal | View Issue Towards bioinspired in vitro models of intestinal mucus Cite this: RSC Adv.,2019,9, 15887 Lorenzo Sardelli, Daniela Peneda Pacheco, Anna Ziccarelli, Marta Tunesi, Omar Caspani, Andrea Fusari, Francesco Briatico Vangosa, Carmen Giordano and Paola Petrini * Intestinal mucus is a biological structure that acts as a barrier between the external environment and the epithelium. It actively selects nutrient and drug intake, regulates the symbiosis with the intestinal microbiota and keeps the epithelium protected from the attack of pathogens. All these functions are closely connected to the chemical and structural complexity of this biological material, on which its viscoelastic and diffusive properties depend. Many models have been proposed to replicate these characteristics using glycoproteins in solution and possibly the addition of other mucus components, such as lipids and other proteins. In the field of mucus modelling, an overall view of the mucus as a material, having its own viscous, rheological and diffusive characteristics, has been undersized with Creative Commons Attribution-NonCommercial 3.0 Unported Licence. Received 28th March 2019 respect to a pure biological-functional analysis. In this review, we propose a description of the mucus as Accepted 9th May 2019 a biomaterial, including a presentation of its chemical and structural complexity, and of its main DOI: 10.1039/c9ra02368b viscoelastic-diffusive properties, in order to provide a synthesis of the characteristics necessary for the rsc.li/rsc-advances engineering of more advanced mucus models. Introduction The European Union has moved towards increasing Replacement, Reduction and Rening (3Rs principle) of animal The intestinal microbial species, present in both physiological studies with other scientically validated alternatives, such as in This article is licensed under a and pathological conditions, affect multiple districts of the vitro models,10 as tools for high throughput screening, limiting human body.
    [Show full text]
  • VIRVĖ SAVO KARTUVĖMS Kapitalistų Sandėriai Su Komunistais Vytautas Meškauskas
    T e oc. oi' 5 □ TL i r. s t r c ba š' 7243 So» Albanv fk., ' yi Chiccęp, III, ‘ 304.29 ; I0TEKA Į -----THE LITHUANIAN NATIONAL NEVVSPAPER -------- P.O. BOX 03206 > 6116 ST. CLAIR AVENUE > CLEVELAND, OHIO 44103 Vol.LXIV Balandis - April 19, 1979 Nr.16 *< TAUTINES MINTIES LIETUVIŲ LAIKRAŠTIS VIRVĖ SAVO KARTUVĖMS Kapitalistų sandėriai su komunistais Vytautas Meškauskas Turiu pasakyti, kad Leninas išpranašavo visą proce­ Konkrečiai kalbant, pereitų są. Leninas, kuris didesnę savo gyvenimo dalį praleido metų prekybos su sovietais Vakaruose, bet ne Rusijoje, kuris geriau pažinojo Vaka­ apyvarta siekė tik 2.8 biijonus rus kaip Rusiją, visados rašė ir sakė, jog Vakarų kapi­ dolerių, t.y. tik trečdalį pre­ talistai padarys viską, kad sustiprintų SSSR ekonomiją. kybos su ... Taiwanu. Biznie­ Jie konkuruos savo tarpe, kad mums parduoti gerybes rius tačiau vilioja ne tiek da­ pigiau ir greičiau, tik tam, kad sovietai jas pirktų ne iš bartinės, kiek ateities galimy­ bės. Šiaip ar taip, Sovietiją vieno, bet iš kito. Jis sakė: jie taip darys negalvodami sudaro rinką su 250 milijonų apie savo pačių ateitį. Vienu sunkiu momentu partijos gyventojų. posėdyje Maskvoje jis drąsino: "Draugai, nepasiduokit Nepaisant to, kad bolševi­ panikai, jei mums pasidarys labai sunku, mes duosime kai konfiskavo visus užsienie­ virvę buržuazijai, ir buržuazija pati pasikars." čių kapitalus, buvusius caro Tada, Kari Radek,... kuris buvo labai sąmojingas, Rusijoje - vien Singerio kom­ paklausė: Vladimire Iličiau, bet iš kur mes paimsime tiek panija prieš karą ten turėjo daug virvės buržuazijos pasikorimui?” Leninas nerūpes­ 27,000 tarnautojų. Vakarų tingai atsakė: "Jie mus ja aprūpins." kapitalistai padėjo sovietų (Iš Aleksandro Solženicyno 1975 m.
    [Show full text]
  • I Identification and Characterization of Martian Acid-Sulfate Hydrothermal
    Identification and Characterization of Martian Acid-Sulfate Hydrothermal Alteration: An Investigation of Instrumentation Techniques and Geochemical Processes Through Laboratory Experiments and Terrestrial Analog Studies by Sarah Rose Black B.A., State University of New York at Buffalo, 2004 M.S., State University of New York at Buffalo, 2006 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirement for the degree of Doctor of Philosophy Department of Geological Sciences 2018 i This thesis entitled: Identification and Characterization of Martian Acid-Sulfate Hydrothermal Alteration: An Investigation of Instrumentation Techniques and Geochemical Processes Through Laboratory Experiments and Terrestrial Analog Studies written by Sarah Rose Black has been approved for the Department of Geological Sciences ______________________________________ Dr. Brian M. Hynek ______________________________________ Dr. Alexis Templeton ______________________________________ Dr. Stephen Mojzsis ______________________________________ Dr. Thomas McCollom ______________________________________ Dr. Raina Gough Date: _________________________ The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. ii Black, Sarah Rose (Ph.D., Geological Sciences) Identification and Characterization of Martian Acid-Sulfate Hydrothermal Alteration: An Investigation
    [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 Sustainability of Habitability on Terrestrial Planets
    PUBLICATIONS Journal of Geophysical Research: Planets REVIEW ARTICLE The sustainability of habitability on terrestrial planets: 10.1002/2016JE005134 Insights, questions, and needed measurements from Mars Special Section: for understanding the evolution of Earth-like worlds JGR-Planets 25th Anniversary B. L. Ehlmann1,2, F. S. Anderson3, J. Andrews-Hanna3, D. C. Catling4, P. R. Christensen5, B. A. Cohen6, C. D. Dressing1,7, C. S. Edwards8, L. T. Elkins-Tanton5, K. A. Farley1, C. I. Fassett6, W. W. Fischer1, Key Points: 2 2 3 9 10 11 2 • Understanding the solar system A. A. Fraeman , M. P. Golombek , V. E. Hamilton , A. G. Hayes , C. D. K. Herd , B. Horgan ,R.Hu , terrestrial planets is crucial for B. M. Jakosky12, J. R. Johnson13, J. F. Kasting14, L. Kerber2, K. M. Kinch15, E. S. Kite16, H. A. Knutson1, interpretation of the history and J. I. Lunine9, P. R. Mahaffy17, N. Mangold18, F. M. McCubbin19, J. F. Mustard20, P. B. Niles19, habitability of rocky exoplanets 21 22 2 1 23 24 25 • Mars’ accessible geologic record C. Quantin-Nataf , M. S. Rice , K. M. Stack , D. J. Stevenson , S. T. Stewart , M. J. Toplis , T. Usui , extends back past 4 Ga and possibly B. P. Weiss26, S. C. Werner27, R. D. Wordsworth28,29, J. J. Wray30, R. A. Yingst31, Y. L. Yung1,2, and to as long ago as 5 Myr after solar K. J. Zahnle32 system formation • Mars is key for testing theories of 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 2Jet Propulsion planetary evolution and processes 3 that sustain habitability
    [Show full text]
  • In Pdf Format
    lós 1877 Mik 88 ge N 18 e N i h 80° 80° 80° ll T 80° re ly a o ndae ma p k Pl m os U has ia n anum Boreu bal e C h o A al m re u c K e o re S O a B Bo l y m p i a U n d Planum Es co e ria a l H y n d s p e U 60° e 60° 60° r b o r e a e 60° l l o C MARS · Korolev a i PHOTOMAP d n a c S Lomono a sov i T a t n M 1:320 000 000 i t V s a Per V s n a s l i l epe a s l i t i t a s B o r e a R u 1 cm = 320 km lkin t i t a s B o r e a a A a A l v s l i F e c b a P u o ss i North a s North s Fo d V s a a F s i e i c a a t ssa l vi o l eo Fo i p l ko R e e r e a o an u s a p t il b s em Stokes M ic s T M T P l Kunowski U 40° on a a 40° 40° a n T 40° e n i O Va a t i a LY VI 19 ll ic KI 76 es a As N M curi N G– ra ras- s Planum Acidalia Colles ier 2 + te .
    [Show full text]
  • The Mars 2020 Candidate Landing Sites: a Magnetic Field Perspective
    The Mars 2020 Candidate Landing Sites: A Magnetic Field Perspective The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Mittelholz, Anna et al. “The Mars 2020 Candidate Landing Sites: A Magnetic Field Perspective.” Earth and Space Science 5, 9 (September 2018): 410-424 © 2018 The Authors As Published http://dx.doi.org/10.1029/2018EA000420 Publisher American Geophysical Union (AGU) Version Final published version Citable link http://hdl.handle.net/1721.1/118846 Terms of Use Creative Commons Attribution-NonCommercial-NoDerivs License Detailed Terms http://creativecommons.org/licenses/by-nc-nd/4.0/ Earth and Space Science RESEARCH ARTICLE The Mars 2020 Candidate Landing Sites: A Magnetic 10.1029/2018EA000420 Field Perspective Key Points: • Mars 2020 offers the opportunity Anna Mittelholz1 , Achim Morschhauser2 , Catherine L. Johnson1,3, to acquire samples that record the Benoit Langlais4 , Robert J. Lillis5 , Foteini Vervelidou2 , and Benjamin P. Weiss6 intensity and direction of the ancient Martian magnetic field 1 • Laboratory paleomagnetic Department of Earth, Ocean and Atmospheric Sciences, The University of British Columbia, Vancouver, British Columbia, 2 3 measurements of returned samples Canada, GFZ German Research Center for Geosciences, Potsdam, Germany, Planetary Science Institute, Tucson, AZ, USA, can address questions about the 4Laboratoire de Planétologie et Geodynamique, UMR 6112 CNRS & Université de Nantes, Nantes, France, 5Space Science history of the
    [Show full text]