POSTER SESSION I: PLANETARY CRYOSPHERES and POLAR PROCESSES III: from MARS to PLUTO 6:00 P.M

Total Page:16

File Type:pdf, Size:1020Kb

POSTER SESSION I: PLANETARY CRYOSPHERES and POLAR PROCESSES III: from MARS to PLUTO 6:00 P.M Lunar and Planetary Science XLVIII (2017) sess306.pdf Tuesday, March 21, 2017 [T306] POSTER SESSION I: PLANETARY CRYOSPHERES AND POLAR PROCESSES III: FROM MARS TO PLUTO 6 :00 p.m. Town Center Exhibit Area Smith I. B. Diniega S. Beaty D. W. Thorsteinsson T. Becerra P. et al. POSTER LOCATION #53 The 6th International Conference on Mars Polar Science and Exploration: State of Knowledge and Top Five Questions [#1701] We discuss the results of the recent 6th International Conference on Mars Polar Science and Exploration and list five questions that synthesize the discussion. Fanara L. Gwinner K. Hauber E. Oberst J. POSTER LOCATION #54 Erosion Rate and Seasonality of Block Falls at the North Pole of Mars Based on HiRISE Images [#2710] We estimate the erosion rate of steep north polar scarps of Mars by identifying active block displacements, their source and their seasonality. Parra S. A. Milkovich S. M. Byrne S. Russell P. S. POSTER LOCATION #55 Variations in Texture of the North Polar Residual Cap of Mars [#1719] 2D FFT analysis on HiRISE imaging of the martian north polar residual cap yields interesting regional and seasonal topographical trends on the textured surface. Diniega S. Hansen C. J. Allen A. Grigsby N. Li Z. et al. POSTER LOCATION #56 Dune-Slope Activity Due to Frost and Wind, Throughout the North Polar Erg, Mars [#2350] After much data / We see autumn frost moves sand / Summer winds erase. Hao J. Michael G. G. van Gasselt S. Jaumann R. POSTER LOCATION #57 Analysis of Spiders in Inca City, Mars: Spatial Distribution and Types [#1712] We mapped the distributions of spiders in the Inca city research area and classified key morphometric features as well as more subtle characteristics. Hansen C. J. Schwamb M. E. Portyankina G. Aye K.-M. POSTER LOCATION #58 Planet Four: Terrains - Araneiform in the South Polar Region of Mars [#2812] Distribution, settings, and morphology of araneiform terrain in the martian south polar region from a citizen science project will be described. Cushing G. E. Titus T. N. POSTER LOCATION #59 THEMIS Observes Early Morning Atmospheric H2O and CO2 Ice on Mars: Preliminary Observations [#2612] In its new early-morning orbit, THEMIS has observed springtime H2O and CO2 ice fogs and clouds in the north polar region, near the retreating seasonal cap. Campbell J. D. Sidiropoulos P. Muller J.-P. POSTER LOCATION #60 Compositional Mapping of the Martian South Polar Residual Cap Using CRISM Infrared Spectra [#2684] Using data from CRISM, we produce maps showing compositional differences in the Mars south polar cap and look for evidence of organic signatures. Whitten J. L. Campbell B. A. POSTER LOCATION #61 Detection of a Subsurface Dome in the South Polar Layered Deposits of Mars [#1255] A dome shaped feature is detected in the subsurface layering in the south polar layered deposits of Mars using SHARAD data. Nerozzi S. Holt J. W. POSTER LOCATION #62 Revealing the Ice Content of the Martian North Polar Basal Unit with SHARAD [#1389] The basal unit / Abundant ice lies within / Not just dusty sand. Lunar and Planetary Science XLVIII (2017) sess306.pdf Holt J. W. Putzig N. E. Nerozzi S. POSTER LOCATION #63 The Chasma Buried Within the North Polar Layered Deposits, Mars [#3038] We detail new information about a major, buried chasma in Planum Boream. Landis M. E. Byrne S. Daubar I. J. Herkenhoff K. E. Dundas C. M. POSTER LOCATION #64 Current Resurfacing Rate of the North Polar Layered Deposits, Mars [#1588] We present current accumulation rates within NPLD craters and numerical modeling results in an effort to generalize these rates to the NPLD surface. Nguyen T. G. Moores J. E. POSTER LOCATION #65 Orientation and Spacing of Small-Scale Surface Features in Mars’ North Polar Cap: Preliminary Results [#2145] Abstract details different small-scale surface features observed on the martian north polar cap to infer possible atmospheric processes that form the features. Sutton S. Byrne S. Herkenhoff K. E. McEwen A. S. POSTER LOCATION #66 Seasonal and Interannual Changes in Meter-Scale Pits in Mars’ North Polar Layered Deposits [#2592] Results from ongoing seasonal and annual observations of changes in meter-scale pits in the NPLD of Mars, and tests of formation hypotheses. Conrad J. W. Abu-Hashmeh N. Nimmo F. White O. L. Singer K. et al. POSTER LOCATION #67 Preliminary Distribution and Statistics of “Bacilli” in the Southern Region of Sputnik Planitia [#1767] Pits called Bacilli / Elliptical by and large / Connecting north south. Williams N. R. Golombek M. P. Bramson A. M. Viola D. Byrne S. et al. POSTER LOCATION #68 Surface Morphologies of Arcadia Planitia as an Indicator of Past and Present Near-Surface Ice [#2852] Morphologic clues / Arcadia Planitia / Where can ice be found? Eason C. Nerozzi S. Holt J. W. POSTER LOCATION #69 Stratigraphic Mapping of the Cavi Unit, Planum Boreum, Mars [#2961] Mars was once warm / It became a lot colder… / The cavi is key. Soare R. J. Conway S. J. Gallagher C. J. Dohm J. M. Williams J. P. et al. POSTER LOCATION #70 Pre- and Post-Periglacial Periglaciation in Utopia Planitia, Mars [#1473] We report the genetic-relationship of ice-rich mantles/clastically-sorted/non-sorted polygons/metre-decametre deep, rimless tiered-depressions (Utopia Planitia). Harrison T. N. Stuurman C. M. Osinski G. R. Tornabene L. L. POSTER LOCATION #71 Deposition and Erosion of the Scalloped Depression Bearing Terrain in Western Utopia Planitia, Mars [#1500] Thick deposits of / Ice and dust eroding to / Leave scallops behind. Head J. W. III Fastook J. L. Palumbo A. M. Denton C. A. Marchant D. R. POSTER LOCATION #72 Late Noachian Icy Highlands Equilibirum Line Altitude (ELA): Predicted Characteristics, Glacial and Periglacial Processes, and Response to Climate Change [#1540] Late Noachian icy highlands equilibrium line altitude environments include cold-based glaciers, proglacial loess plateaus, and punctuated fluvial/lacustrine. Fastook J. L. Head J. W. POSTER LOCATION #73 Hellas Basin Rim and Wall Glaciation in the Late Noachian: Enhanced Flow, Basal Melting, Wet-Based Glaciation and Erosion, and Generation and Fate of Meltwater in the Ablation Zone [#1735] An ice sheet model that simulates flow from the rim of Hellas Crater into its interior, where warmer temperatures coupled with thick ice allow for a melted bed. Lunar and Planetary Science XLVIII (2017) sess306.pdf Pathare A. V. Joseph E. C. S. Crown D. A. Chuang F. C. Berman D. C. et al. POSTER LOCATION #74 Glacial Flow Within Martian Lobate Debris Aprons: Evidence from Surface Texture Mapping in Eastern Hellas [#2859] We present surface texture mapping evidence for widespread small-scale glacial flow features within lobate debris aprons in the eastern Hellas region of Mars. Guallini L. Pauselli C. Brozzetti F. Marinangeli L. Thomas N. POSTER LOCATION #75 Thermal Modeling of Large-Scale Deformational Systems in the South Polar Layered Deposits (Promethei Lingula, Mars): Geologic Constraints [#1899] SPLD in Promethei Lingula (Mars) are locally affected by deformations. We performed thermal analysis to understand their rheology and compositional variations. Guallini L. Parker T. J. Sutton S. Thomas N. POSTER LOCATION #76 Esker-Like Ring-Shaped Ridges in Peta, Novara, and Two Other Unnamed Craters on Mars: Evidences of Ancient Glaciers? [#1959] Peta, Novara and two other craters in low-latitude regions on Mars show ring-shaped ridges that we interpret to be eskers formed by melting of ancient glaciers. Rutledge A. M. Scudder N. A. Havig J. R. Horgan B. Rampe E. B. et al. POSTER LOCATION #77 Does Melt-Driven Silica Cycling Dominate Weathering in Glaciated Volcanic Terrains? [#2069] Mobile silica, glaciated mafic rocks: Important for Mars. Kirchoff M. R. Grimm R. E. POSTER LOCATION #78 Preservation of Tropical Subsurface Ice into the Very Recent History of Mars [#2857] Young formation model ages of single layered ejecta craters indicate current tropical subsurface ice on Mars. Butcher F. E. G. Gallagher C. Arnold N. S. Balme M. R. Conway S. J. et al. POSTER LOCATION #79 Morphometric Characterisation of Eskers Associated with an Extant Mid-Latitude Glacier on Mars [#1238] Water under Mars / Mid-lat glacier left clues / On recent melting. Baker D. M. H. Carter L. M. POSTER LOCATION #80 Probing the Near Surface of Glacial Deposits on Mars [#2650] The complete range of crater morphologies on martian glacial deposits are assessed to evaluate the physical properties and structure of supraglacial debris. Petersen E. I. Holt J. W. Levy J. S. Goudge T. A. POSTER LOCATION #81 New Constraints on Surface Debris Layer Composition for Martian Mid-Latitude Glaciers from SHARAD and HiRISE [#2767] Glacial cake of Mars / Topped up with frosty icing! / May radar see thee? Manchester A. Byers G. Guerrero M. McGrath S. Nasser A. POSTER LOCATION #82 Examination of Effects of Impact Driven Tectonics on Surface Activity of Asteroids and Icy Worlds [#1586] We hypothesize that large craters correlated with linear features are evidence of impact-driven tectonics observed on both icy asteroids and icy moons. .
Recommended publications
  • MID-LATITUDE MARTIAN ICE AS a TARGET for HUMAN EXPLORATION, ASTROBIOLOGY, and IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A
    First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1011.pdf MID-LATITUDE MARTIAN ICE AS A TARGET FOR HUMAN EXPLORATION, ASTROBIOLOGY, AND IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A. S. McEwen1, and C. M. Dundas2. 1University of Arizona, Department of Planetary Sciences, 2USGS, Astrogeology Science Center. Introduction: Future human missions to Mars will region of late Noachian highlands terrain, and is com- need to rely on resources available near the Martian prised of a series of grabens and ridges surrounded by surface. Water is of primary importance, and is known later Hesperian/Amazonian lava flows from the Thar- to be abundant on Mars in multiple forms, including sis region [7]. The proposed landing site is within these hydrated minerals [1] and pore-filling and excess ice lava flows (HAv), and provides access to a region of deposits [2]. Of these sources, excess ice (or ice which late Hesperian lowlands in the western region of the exceeds the available regolith pore space) may be the EZ. There is evidence for Amazonian glacial and peri- most promising for in-situ resource utilization (ISRU). glacial activity [e.g., HiRISE images Since Martian excess ice is thought to contain a low PSP_008671_2210 and ESP_017374_2210], and the fraction of dust and other contaminants (~<10% by Gamma Ray Spectrometer water map suggests that volume, [3]) only a modest deposit of excess ice will there is abundant subsurface ice in the uppermost me- be sufficient to support a human presence. ter within this region [10]. Meandering channel-like Subsurface water ice may also be of astrobiological features have been identified in HiRISE images (e.g., interest as a potential current habitat or as a preserva- PSP_003529_2195 in close proximity to apparent ice tion medium for biosignatures.
    [Show full text]
  • Case Fil Copy
    NASA TECHNICAL NASA TM X-3511 MEMORANDUM CO >< CASE FIL COPY REPORTS OF PLANETARY GEOLOGY PROGRAM, 1976-1977 Compiled by Raymond Arvidson and Russell Wahmann Office of Space Science NASA Headquarters NATIONAL AERONAUTICS AND SPACE ADMINISTRATION • WASHINGTON, D. C. • MAY 1977 1. Report No. 2. Government Accession No. 3. Recipient's Catalog No. TMX3511 4. Title and Subtitle 5. Report Date May 1977 6. Performing Organization Code REPORTS OF PLANETARY GEOLOGY PROGRAM, 1976-1977 SL 7. Author(s) 8. Performing Organization Report No. Compiled by Raymond Arvidson and Russell Wahmann 10. Work Unit No. 9. Performing Organization Name and Address Office of Space Science 11. Contract or Grant No. Lunar and Planetary Programs Planetary Geology Program 13. Type of Report and Period Covered 12. Sponsoring Agency Name and Address Technical Memorandum National Aeronautics and Space Administration 14. Sponsoring Agency Code Washington, D.C. 20546 15. Supplementary Notes 16. Abstract A compilation of abstracts of reports which summarizes work conducted by Principal Investigators. Full reports of these abstracts were presented to the annual meeting of Planetary Geology Principal Investigators and their associates at Washington University, St. Louis, Missouri, May 23-26, 1977. 17. Key Words (Suggested by Author(s)) 18. Distribution Statement Planetary geology Solar system evolution Unclassified—Unlimited Planetary geological mapping Instrument development 19. Security Qassif. (of this report) 20. Security Classif. (of this page) 21. No. of Pages 22. Price* Unclassified Unclassified 294 $9.25 * For sale by the National Technical Information Service, Springfield, Virginia 22161 FOREWORD This is a compilation of abstracts of reports from Principal Investigators of NASA's Office of Space Science, Division of Lunar and Planetary Programs Planetary Geology Program.
    [Show full text]
  • Widespread Excess Ice in Arcadia Planitia, Mars 10.1002/2015GL064844 Ali M
    PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Widespread excess ice in Arcadia Planitia, Mars 10.1002/2015GL064844 Ali M. Bramson1, Shane Byrne1, Nathaniel E. Putzig2, Sarah Sutton1, Jeffrey J. Plaut3, 4 4 Key Points: T. Charles Brothers , and John W. Holt • Terraced craters: abundant in Arcadia 1 2 Planitia, indicate subsurface layering Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA, Southwest Research Institute, Boulder, • A widespread subsurface interface is Colorado, USA, 3Jet Propulsion Laboratory, Pasadena, California, USA, 4Institute for Geophysics, University of Texas at also detected by SHARAD Austin, Austin, Texas, USA • Combining data sets yields dielectric constants consistent with decameters of excess water ice Abstract The distribution of subsurface water ice on Mars is a key constraint on past climate, while the volumetric concentration of buried ice (pore-filling versus excess) provides information about the process Supporting Information: that led to its deposition. We investigate the subsurface of Arcadia Planitia by measuring the depth of terraces • Table S1, Texts S1–S3, and fl Figures S1–S3 in simple impact craters and mapping a widespread subsurface re ection in radar sounding data. Assuming that the contrast in material strengths responsible for the terracing is the same dielectric interface that causes Correspondence to: the radar reflection, we can combine these data to estimate the dielectric constant of the overlying material. We A. M. Bramson, compare these results to a three-component dielectric mixing model to constrain composition. Our results [email protected] indicate a widespread, decameters-thick layer that is excess water ice ~104 km3 in volume. The accumulation and long-term preservation of this ice is a challenge for current Martian climate models.
    [Show full text]
  • GEOLOGIC MAPS of the OLYMPUS MONS REGION of MARS by Elliot C. Morris and Kenneth L. Tanaka
    U.S. DEPARTMENT OF THE INTERIOR U.S. GEOLOGICAL SURVEY GEOLOGIC MAPS OF THE OLYMPUS MONS REGION OF MARS By Elliot C. Morris and Kenneth L. Tanaka Prepared for the NATIONAL AERONAUTICS AND SPACE ADMINISTRATION ..... t\:) a 0 a0 0 0 )> z 0 ..... ..... MISCELLANEOUS INVESTIGATIONS SERIES a 0 Published by the U.S. Geological Survey, 1994 a0 0 0 3: ~ U.S. DEPARTMENT OF THE INTERIOR TO ACCOMPANY MAP I-2327 U.S. GEOLOGICAL SURVEY GEOLOGIC MAPS OF THE OLYMPUS MONS REGION OF MARS By Elliot C. Morris and Kenneth L. Tanaka INTRODUCTION measurements of relief valuable in determining such factors as Olympus Mons is one of the broadest volcanoes and volcano volume, structural offsets, and lava-flow rheology. certainly the tallest in the Solar System. It has been extensively Except for the difference in extent of the areas mapped, the described and analyzed in scientific publications and frequently topographic information, the cartographic control (latitudes noted in the popular and nontechnical literature of Mars. and longitudes of features may differ by as much as a few tenths However, the first name given to the feature-Nix Olympica of a degree), and the greater detail permitted by the larger scale (Schiaparelli, 1879)-was based on its albedo, not its size, base, the two maps are virtually the same. A comparison of our because early telescopic observations of Mars revealed only map units with those of other Viking-based maps is given in albedo features and not topography (lnge and others, 1971). table 1. After Mariner 9 images acquired in 1971 showed that this Unravellng the geology of the Olympus Mons region is not albedo feature coincides with a giant shield volcano (McCauley limited to a simple exercise in stratigraphy.
    [Show full text]
  • Preservation of Midlatitude Ice Sheets on Mars 10.1002/2017JE005357 A
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Preservation of Midlatitude Ice Sheets on Mars 10.1002/2017JE005357 A. M. Bramson1 , S. Byrne1 , and J. Bapst1,2 Key Points: 1Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA, 2Department of Earth and Space Sciences, • Decameters of ice loss over the past 21 Myr form a sublimation lag, University of Washington, Seattle, WA, USA allowing Mars midlatitude ice sheets ~100 m thick to survive to present • Retreat of this ice could have Abstract Excess ice with a minimum age of tens of millions of years is widespread in Arcadia Planitia on contributed 6% of the north polar Mars, and a similar deposit has been found in Utopia Planitia. The conditions that led to the formation and layered deposits in the last 4 Myr and over 10% if polar deposits are older preservation of these midlatitude ice sheets hold clues to past climate and subsurface structure on Mars. We • Modeling of vapor migration suggests simulate the thermal stability and retreat of buried excess ice sheets over 21 Myr of Martian orbital solutions that ice porosity can be sustained on and find that the ice sheets can be orders of magnitude older than the obliquity cycles that are typically timescales longer than retreat, consistent with radar observations thought to drive midlatitude ice deposition and sublimation. Retreat of this ice in the last 4 Myr could have contributed ~6% of the volume of the north polar layered deposits (NPLD) and more than 10% if the NPLD are older than 4 Myr. Matching the measured dielectric constants of the Arcadia and Utopia Planitia deposits requires ice porosities of ~25–35%.
    [Show full text]
  • Surface Morphologies of Arcadia Planitia As an Indicator of Past and Present 1 1 2 2 2 Near-Surface Ice
    Lunar and Planetary Science XLVIII (2017) 2852.pdf SURFACE MORPHOLOGIES OF ARCADIA PLANITIA AS AN INDICATOR OF PAST AND PRESENT 1 1 2 2 2 NEAR-SURFACE ICE. N. R. Williams , M. P. Golombek , A. M. Bramson , D. Viola , S. Byrne , A. S. McEw- en2, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, 2University of Arizona, Tucson, AZ 85721. Introduction: The occurrence of water on Mars Results: Out of the 230 images surveyed, 165 im- holds key records for the planet’s past and present cli- ages contain polygonal terrain, 86 images contain mate. Polar caps are the most obvious large-scale ex- crenulated terrain, and 36 images contain pitted terrain amples of water-ice on Mars today, but a latitude- (Fig. 2). Polygonal terrain is the most widespread, with dependent mantle (LDM) of shallow water-ice has also very few examples at <36°N (in 1 of 34 images, Fig. 2) been remotely observed at 30°N-40°N. Ice is not stable but becoming ubiquitous above 40°N (in 96 of 100 at these mid-latitudes today, but is expected to have images, Fig. 2). Crenulated terrain primarily occurs in a precipitated in the past during different obliquities and narrow latitude band between 38°N and 43°N (median climatic conditions [1] with residual excess ice likely 39.6°N), with a few outlier crenulated areas also found preserved in the subsurface. around the lobate debris aprons on the west side of the Arcadia Planitia, in particular, is a generally flat- surveyed area. Pitted terrain primarily occurs poleward lying region around ~200°E, ~40°N where several of 40°N often in association with polygons, with a few studies suggest a widespread abundance of shallow ice.
    [Show full text]
  • Durham Research Online
    Durham Research Online Deposited in DRO: 27 March 2019 Version of attached le: Published Version Peer-review status of attached le: Peer-reviewed Citation for published item: Orgel, Csilla and Hauber, Ernst and Gasselt, Stephan and Reiss, Dennis and Johnsson, Andreas and Ramsdale, Jason D. and Smith, Isaac and Swirad, Zuzanna M. and S¡ejourn¡e,Antoine and Wilson, Jack T. and Balme, Matthew R. and Conway, Susan J. and Costard, Francois and Eke, Vince R. and Gallagher, Colman and Kereszturi, Akos¡ and L osiak, Anna and Massey, Richard J. and Platz, Thomas and Skinner, James A. and Teodoro, Luis F. A. (2019) 'Grid mapping the Northern Plains of Mars : a new overview of recent water and icerelated landforms in Acidalia Planitia.', Journal of geophysical research : planets., 124 (2). pp. 454-482. Further information on publisher's website: https://doi.org/10.1029/2018JE005664 Publisher's copyright statement: Orgel, Csilla, Hauber, Ernst, Gasselt, Stephan, Reiss, Dennis, Johnsson, Andreas, Ramsdale, Jason D., Smith, Isaac, Swirad, Zuzanna M., S¡ejourn¡e,Antoine, Wilson, Jack T., Balme, Matthew R., Conway, Susan J., Costard, Francois, Eke, Vince R., Gallagher, Colman, Kereszturi, Akos,¡ L osiak, Anna, Massey, Richard J., Platz, Thomas, Skinner, James A. Teodoro, Luis F. A. (2019). Grid Mapping the Northern Plains of Mars: A New Overview of Recent Water and IceRelated Landforms in Acidalia Planitia. Journal of Geophysical Research: Planets 124(2): 454-482. 10.1029/2018JE005664. To view the published open abstract, go to https://doi.org/ and enter the DOI. Additional information: Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.
    [Show full text]
  • Observations of Martian Gullies and Constraints on Potential Formation Mechanisms II
    Icarus 188 (2007) 324–344 www.elsevier.com/locate/icarus Observations of martian gullies and constraints on potential formation mechanisms II. The northern hemisphere Jennifer L. Heldmann a,∗, Ella Carlsson b,c, Henrik Johansson b, Michael T. Mellon d, Owen B. Toon e a NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA b Division of Physics, Luleå University of Technology, SE-97187 Luleå, Sweden c Swedish Institute of Space Physics, Box 812, SE-98128 Kiruna, Sweden d University of Colorado, Laboratory for Atmospheric and Space Physics, Boulder, CO 80309, USA e University of Colorado, Laboratory for Atmospheric and Space Physics, Program in Atmospheric and Oceanic Sciences, Boulder, CO 80309, USA Received 12 May 2006; revised 9 November 2006 Available online 3 January 2007 Abstract The formation process(es) responsible for creating the observed geologically recent gully features on Mars has remained the subject of intense debate since their discovery. We present new data and analysis of northern hemisphere gullies from Mars Global Surveyor data which is used to test the various proposed mechanisms of gully formation. We located 137 Mars Orbiter Camera (MOC) images in the northern hemisphere that contain clear evidence of gully landforms and analyzed these images in combination with Mars Orbiter Laser Altimeter (MOLA) and Thermal Emission Spectrometer (TES) data to provide quantitative measurements of numerous gully characteristics. Parameters we measured include apparent source depth and distribution, vertical and horizontal dimensions, slopes, orientations, and present-day characteristics that affect local ground temperatures. Northern hemisphere gullies are clustered in Arcadia Planitia, Tempe Terra, Acidalia Planitia, and Utopia Planitia.
    [Show full text]
  • Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)
    ASTROBIOLOGY Volume 14, Number 11, 2014 News & Views ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2014.1227 A New Analysis of Mars ‘‘Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2) John D. Rummel,1 David W. Beaty,2 Melissa A. Jones,2 Corien Bakermans,3 Nadine G. Barlow,4 Penelope J. Boston,5 Vincent F. Chevrier,6 Benton C. Clark,7 Jean-Pierre P. de Vera,8 Raina V. Gough,9 John E. Hallsworth,10 James W. Head,11 Victoria J. Hipkin,12 Thomas L. Kieft,5 Alfred S. McEwen,13 Michael T. Mellon,14 Jill A. Mikucki,15 Wayne L. Nicholson,16 Christopher R. Omelon,17 Ronald Peterson,18 Eric E. Roden,19 Barbara Sherwood Lollar,20 Kenneth L. Tanaka,21 Donna Viola,13 and James J. Wray22 Abstract A committee of the Mars Exploration Program Analysis Group (MEPAG) has reviewed and updated the description of Special Regions on Mars as places where terrestrial organisms might replicate (per the COSPAR Planetary Protection Policy). This review and update was conducted by an international team (SR-SAG2) drawn from both the biological science and Mars exploration communities, focused on understanding when and where Special Regions could occur. The study applied recently available data about martian environments and about terrestrial organisms, building on a previous analysis of Mars Special Regions (2006) undertaken by a similar team. Since then, a new body of highly relevant information has been generated from the Mars Reconnaissance Orbiter (launched in 2005) and Phoenix (2007) and data from Mars Express and the twin Mars Exploration Rovers (all 2003).
    [Show full text]
  • Modern Mars' Geomorphological Activity
    Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, Matthew Chojnacki, Susan Conway, Colin Dundas, Candice Hansen, Alfred Mcewen, et al. To cite this version: Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, et al.. Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity. Geomorphology, Elsevier, 2021, 380, pp.107627. 10.1016/j.geomorph.2021.107627. hal-03186543 HAL Id: hal-03186543 https://hal.archives-ouvertes.fr/hal-03186543 Submitted on 31 Mar 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. 1 Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity 2 3 Authors: Serina Diniega1,*, Ali M. Bramson2, Bonnie Buratti1, Peter Buhler3, Devon M. Burr4, 4 Matthew Chojnacki3, Susan J. Conway5, Colin M. Dundas6, Candice J. Hansen3, Alfred S. 5 McEwen7, Mathieu G. A. Lapôtre8, Joseph Levy9, Lauren Mc Keown10, Sylvain Piqueux1, 6 Ganna Portyankina11, Christy Swann12, Timothy N. Titus6,
    [Show full text]
  • Spaceflight Engineering 2018 Landing Sites.Key
    Spaceflight Engineering 2018 Landing Sites Landing Site #1: Schiaparelli Crater The Schiaparelli Crater is a large impact crater on Mars, located in the Sinus Sabaeus quadrangle. Coordinates: (2.71ºS, 16.77ºE) The crater measures 459 km in diameter Landing Site #2: Milankovic Crater The Milankovic crater is another large impact crater on Mars. It is located much further north than the Schiaparelli crater, in the flat plain of Vastitas Borealis. Coordinates: (54.7ºN 146.7ºW) The Milankovic crater is 118.4km in diameter Landing Site #3: Arcadia Planitia The Arcadia Planitia is a large flat plains region in the northern hemisphere of Mars. It lies just south of the northern polar ice cap. Coordinates: (47.2ºN 184.3ºE) This area has been a particular interest for many scientists because the possibility of ground ice has led to discussion about water. Location and Setting: Ismenius Cavus Mission statement: Your company’s mission goes here Location and Setting: Aram Chaos Coord: 2.8°N, 338.9°E Elevation: 3.4 km - A crater that once contained water -Clay minerals consistent with fine-grained deposits at lake bottom ● -Past habitability in subsurface environment -Hesperian atmosphere preservation– evaporite minerals Location and Setting: Hellas Chasma Coord:Mission 34.64°S 65.47°E statement: Hellas Chasma is a deep, elongated, Yoursteep-sided company’s depression 148 KM Diameter Notmission much known about it. goes here Purpose To earn more about Mars’ Hesperian period and fluvial activity Examine sediments Biggest impact crater Advantages Research done on distance and time away from other sites in the Hellas Basin It suggests fluvial activity Largest impact crater, may be able to learn more Disadvantages Very little research done on Hellas Chasma May be an interesting site, but not much to go off of other than geomorphology Planum Boreum • Northern polar plain on Mars • Around 1.5x size of Texas • Permanent ice cap with several different layers • Spirals in land formed from katabatic wind 87.32ºN 54.96ºE -8,520 ft.
    [Show full text]
  • 15. Volcanic Activity on Mars
    15. Volcanic Activity on Mars Martian volcanism, preserved at the surface, composition), (2) domes and composite cones, is extensive but not uniformly distributed (Fig. (3) highland paterae, and related (4) volcano- 15.1). It includes a diversity of volcanic land- tectonic features. Many plains units like Lu- forms such as central volcanoes, tholi, paterae, nae Planum and Hesperia Planum are thought small domes as well as vast volcanic plains. to be of volcanic origin, fed by clearly defined This diversity implies different eruption styles volcanoes or by huge fissure volcanism. Many and possible changes in the style of volcanism small volcanic cone fields in the northern plains with time as well as the interaction with the are interpreted as cinder cones (Wood, 1979), Martian cryosphere and atmosphere during the formed by lava and ice interaction (Allen, evolution of Mars. Many volcanic constructs 1979), or as the product of phreatic eruptions are associated with regional tectonic or local (Frey et al., 1979). deformational features. An overview of the temporal distribution of Two topographically dominating and mor- processes, including the volcanic activity as phologically distinct volcanic provinces on Mars well as the erosional processes manifested by are the Tharsis and Elysium regions. Both are large outflow channels ending in the northern situated close to the equator on the dichotomy lowlands and sculpting large units of the vol- boundary between the cratered (older) high- canic flood plains has been given by Neukum lands and the northern lowlands and are ap- and Hiller (1981). This will be discussed in proximately 120◦ apart. They are characterized this work together with new findings.
    [Show full text]