AQUEOUS SEDIMENTARY DEPOSITS IN HOLDEN CRATER: LANDING SITE FOR THE MARS SCIENCE LABORATORY Rossman P. Irwin III and John A. Grant Smithsonian Institution,

Slides:

Advertisements

Similar presentations

Remaining Uncertainties: Little evidence for shorelines corresponding to the elevation of the delta surface and the spillway to the eastern basin, though.

Advertisements

Mars: First Order Landscapes The Great Crustal Dichotomy

Bankfull / Effective / Dominant

1 The Hesperian. 2 What’s important in the Late Noachian/Hesperian/Early Amazonian? Impact rate declining rapidly Volcanic resurfacing at a maximum? Hesperian.

MSL Parker and BargeFriday, June 2, 2006 Landing Site Map Compilation for MSL Tim Parker, JPL Laurie Barge, USC.

Martian Craters with Interior Deposits: Global Survey Results and Wind Model P21D-1875 Kristen A. Bennett 1 and Mark Schmeeckle 2 1 School of Earth and.

Mars Global Surveyor Mars Orbiter Camera 8 May 2006 Confidential and Proprietary Material of MSSS. This document may contain information subject to the.

Remaining Uncertainties: Is there evidence of a shoreline/bench in Eberswalde crater corresponding to the elevation of the delta surface and the spillway.

The Light-toned Sediments in and near lower Mawrth Vallis are a Drape Deposit Alan D. Howard Jeffrey M. Moore.

The Valley Network Record on Mars (Class 1). Challenges for our understanding: Climate models have a very hard time raising the Martian surface temperature.

Alluvial Fan Science Potential Kelin X. Whipple and Kelli Wakefield School of Earth and Space Exploration Arizona State University.

Large craters outside the ellipse Long/lat (by decreasing size): E, 24.24N E, 24.30N E, 24.25N E, 24.32N E,

National Center for Earth-surface Dynamics Modeling physical and ecological dynamics of channel systems that shape Earth’s surface Moving boundary problems.

Valleys & inverted valleys in Mawrth Vallis flank Long/lat: E, 24.11N E, 24.06N E, 24.04N E, 23.99N E, 24.17N.

Oyama layered deposits Long/lat: from E, 24.00N to E, 23.20N Rational: Clays have been transported onto the floor of Oyama and deposited as.

C.M. Rodrigue, 2007 Geography, CSULB Mars: First Order Landscapes Geography S/07 Dr. Christine M. Rodrigue.

Light-toned paleo-surface Long/lat: E, 23.76N Rational: During the deposition of the layered unit, a layer may have remained at the surface for a.

ExoMars LSEC 2018 Landing Site Engineering Constraints LSSWS# December 2014 L. Lorenzoni and ExoMars Project.

Mapping the Surface of Mars NOAO Science Education Group and Chris Martin from Howenstine Magnet High School.

Stream Channels. There is some overlap of Earth and Mars surface conditions Worst of Mars Worst of Earth.

Landing Site Thermal Minima for Rover Lifetime Concerns Nathan T. Bridges and Terry Z. Martin Jet Propulsion Laboratory Significant acknowledgments to.

Northwestern Slope Valleys (NSVS): Prime Candidate Site For MSL Exploration Of Mars J.M. Dohm, R.C. Anderson, V Baker, T.M. Hare, S.J. Wheelock.

Discussion of High Thermal Inertia Craters on Mars in the Isidis and Syrtis Major Regions Jordana Friedman Arizona State University.

MSL Science Team Landing Sites Discussions — Gale CraterEdgett, p. 1 Gale Crater MSL Candidate Landing Site in Context by K. Edgett April 2010.

Sharon Wilson, Smithsonian Institution Alan Howard, University of Virginia Jeff Moore, NASA Ames Research Center Terby Crater Terby Crater First MSL Landing.

The Solar System a1 Mercury Sun Venus Earth Mars Asteroids Jupiter Saturn Uranus Neptune Other objects Observe our solar system Four inner planets.

PROPOSED 2018 Joint Rover Mission Plans for Proposed 2018 NASA & ESA Joint Rover Mission Landing Site Selection Matt Golombek Mars Exploration Program.

NASA’s Exploration Plan: “Follow the Water” GEOLOGY LIFE CLIMATE Prepare for Human Exploration When Where Form Amount WATER NASA’s Strategy for Mars Exploration.

Preservation of Evidence of Ancient Environments and Life on Mars

PROPOSED EXPLORATION ZONE TITLE Workshop Abstract # AUTHOR(s) with AFFILIATIONS.

Fluvial Deposits in Margaritifer Basin Kevin K. Williams and John A. Grant Center for Earth and Planetary Studies, Smithsonian Institution Corey M. Fortezzo.

Lava Flows of Arsia Mons, Mars Ruben Rivas College of Engineering University of Arizona (Tucson, Az) Space Grant Mentor: David Crown Planetary Science.

Interlude  Viking mission operations ended in the early 1980s  Viking missions gave scientists the most complete picture of Mars to date. What does this.

Mars Science Laboratory Landing Site Workshop 1 Xanthe-Hellas-Elysium-Isidis LSC / 01 / 06/06 NMMNHS 1 Four Proposed Mars Science Laboratory Landing Sites.

MSL Science Team Field Site Discussions — Eberswalde CraterEdgett, p. 1 Eberswalde Crater MSL Candidate Field Site in Context by K. Edgett, 9 June 2010.

Software used: ArcMap , MatLab R2015b, Google Earth 7.1.5

C.M. Rodrigue, 2014 Geography, CSULB Mars: Fourth Order Landscapes Geography 441/541 S/14 Dr. Christine M. Rodrigue.

PROPOSED MARS LANDING SITES FOR MER A & B West Hemisphere Centered at: 30°N, 30°W East Hemisphere Centered at: 30°N, 210°W 10°N 15°S 0° O OO O O 10°N 15°S.

Mars Rover Exploration at Gusev Crater and Back-Ups Characterization and Science Potential of the Sites 2nd 2003 Landing Site Workshop, Pasadena, Ca, Oct.

East Melas Chasma: Insight into Valles Marineris Matt Chojnacki & Brian Hynek Laboratory for Atmospheric and Space the University of Colorado.

The Gale Crater Mound: A Candidate Landing Site for the 2009 Mars Science Laboratory Jim Bell 1, Ken Edgett 2, Scott Rowland 3, Mike Malin 2 Representing.

Determining surface characteristics at candidate MSL landing sites using THEMIS high-resolution orbital thermal inertia data Robin Fergason Philip Christensen.

Did Lava or Water Affect the Formation of Elysium Planitia?

Enabling Capabilities A Robotic Field Geologist Access to a site mapped from orbit Long life, mobility, capability to explore a local region Remote sensing.

REGOLITH LANDFORM MAPPING OF MERIDIANI PLANUM AND SURROUNDS J. D. A. Clarke 1 C. F. Pain 2 and M. Thomas 1, 1 Australian Centre for Astrobiology, Macquarie.

Mars Science Laboratory 1st Landing Site Workshop Pasadena, CA — 31 May – 2 June Fine-layered Meridiani crater for the MSL Landing Site L. V. Posiolova,

NAI Mars Focus Group Videocon Science and Landing Site Priorities for the Mars 2003 Mission Presentations by: n Ronald Greeley (ASU) & Ruslan Kuzmin (Vernadsky.

SEDIMENTARY ROCKS AND METHANE – SOUTHWEST ARABIA TERRA Carlton Allen and Dorothy Oehler NASA Johnson Space Center Houston, TX Elizabeth Venechuk Scripps.

A Wealth of Opportunities The signature of water is pervasive in and around the proposed ellipse, which resides ~600 km ENE of Opportunity –Ellipse: Over.

TRAVERSE ACROSS LOWER STRATA OF MERIDIANI PLANUM LAYERED DEPOSITS Alan D. Howard Department of Environmental Sciences University of Virginia Jeffrey M.

Sinus Meridiani (Hematite) Landing Site for 2003 MER Phil Christensen & The TES Science Team Presentation to NAI MWG by Vicky Hamilton 8 January 2001.

MAPPING MARS CRATER LANDING SITES & MODELLING CRATER DYNAMICS COMPUTERS IN GEOLOGY TERM PROJECT STEPHANIE SHAHRZAD NOVEMBER 7, 2015.

Gale Crater Stratigraphic Measurements and Preliminary Interpretations Ryan Anderson April, 2009.

Multidecadal Changes in Aeolian Morphology around Gale Crater using datasets of Mars Color Camera and other Orbiters Resource Person ISRO - Dr. A S Arya.

Boundary layer models of Martian hydrothermal systems Kate Craft 11/2/2007.

Remaining Uncertainties: Little evidence of a shoreline/bench in Eberswalde crater corresponding to the elevation of the delta surface and the spillway.

Mars Exploration Rover Geological Diversity within 500 m Radius MER Landing Spots: Comparison Among Landing Ellipses Robert Sullivan Jon Branscomb R. Alan.

Aqueous Alteration and Habitability in Nili Fossae J.F. Mustard, F. Poulet, N. Mangold, J-P. Bibring, R.E. Milliken, S. Pelkey, and L. Kanner Noachian.

Introduction: The Mawrth Vallis region has been identified by the Mars Express OMEGA and MRO CRISM instruments as a region with abundant hydrated phyllosilicate.

Visit NE Syrtis Major! Win Valuable Martian Geological History! Ralph P. Harvey Case Western Reserve University Planetary Time Share Specialist Ralph P.

C.M. Rodrigue, 2016 Geography, CSULB Mars: Second Order Landscapes Geography 441/541 S/16 Dr. Christine M. Rodrigue.

Wet environment reconstruction using IR spectra on Mars Akos Kereszturi Konkoly Astronomical Institute, MTA CSFK Mars Astrobiology Group (ESA RCL) OTKA.

Deciphering Crater-bound Alluvial Fans in Margaritifer Terra

Preservation of Evidence of Ancient Environments and Life on Mars

Impact Crater Lakes and the Astrobiological Exploration of Mars

Predicting the hydrologic and water quality implications of climate and land use change in forested catchments Dennis P. Lettenmaier Department of Civil.

The Nature and Origin of Deposits in Uzboi Vallis

Geomorphology of Eastern Meridiani Planum

Holden NE crater Main Goals:

Stratigraphic Analysis of the Distributary Fan in Holden NE Crater

Presentation transcript:

AQUEOUS SEDIMENTARY DEPOSITS IN HOLDEN CRATER: LANDING SITE FOR THE MARS SCIENCE LABORATORY Rossman P. Irwin III and John A. Grant Smithsonian Institution, National Air and Space Museum

REGIONAL SETTING 150 km

LOCAL SETTING 50 km

THEMIS DAY IR WITH MOLA Most of the dissection and deposits are on the high- relief western crater rim. Note the low- thermal- inertia region in the crater center, contrast with outlying floor surfaces. 25 km

THEMIS NIGHT IR MOSAIC 25 km

HOLDEN CRATER: JUSTIFICATION Alluvial fans: weathering and transport processes, discharge and runoff production rates inferred from sedimentary load and structures. Light-toned layered deposits: composition, origin, environmental implications. Habitability? Paleoclimate of the Late Noachian to Early Hesperian transition. Discharge from an exterior drainage network. Relatively safe landing zone bordering areas of interest within range of the rover. Impact ejecta from 2.5 km crater in landing zone. HOLDEN CRATER: JUSTIFICATION

AGE OF HOLDEN CRATER 50 km

ALLUVIAL FANS 15 km

ALLUVIAL FANS 10 km

ALLUVIAL FANS Fan is 13 km across

ALLUVIAL FANS MOC E km across

UZBOI VALLIS DEPOSIT 5 km

LANDING AREA Zone is 20 km across

AREA OF INTEREST: 2 RADII Zone is 20 km across

HYDROLOGY Calculate critical shear stress for entrainment τ c given largest sediment grain diameter D: τ c = 0.06(ρ s  ρ w )gD Solve for flow depth H at that shear stress given measured slope S: τ = ρ w gHS Solve for discharge Q given channel width W: Q = HWV = H 1.5 W(8gS/f) 0.5 ρ s is sediment density, ρ w is fluid density, g is gravitational acceleration 1 km

MOC E km across LAYERED DEPOSITS MOC M km across

MOC E km across LIGHT-TONED LAYERED DEPOSITS

MOC E km across LIGHT-TONED LAYERED DEPOSITS

LANDING AREA MOC E km across

ENGINEERING REQUIREMENTS Engineering Parameter RequirementObservationsNotes Latitude60°N to 60°S26.4°S Altitude≤ 2000 m–2230 to –2330MOLA-derived elevation Landing ellipse radius≤ 10 km10 kmExcluding uncontrolled wind effects during parachute descent Slopes2 to 5 km length scale ≤ 3 degrees<1° in landing area Radar altimetry errors to start powered descent 20 to 40 m length scale ≤ 15 degreesHRSCRadar processing – spoofing 5 m length scale ≤ 15 degreesMOC or HiRISE stereo DEMs? Rover tilting Trafficability in loose granular material Rock height≤ 0.6 mHiRISE (flows likely unable to move this size) Probability that a rock higher than 0.6 m occurs in a random sampled area of 4 m 2 should be less than 0.25%. Suggests low to moderate rock abundance WindsSteady state horizontal ≤ 30 m/sModelsAt altitudes of 0 to 10 km above the surface Steady state vertical ≤ 10 m/sModelsAt altitudes of 0 to 10 km above the surface Wind gustsEvaluate case by case ModelsAt altitudes of 0 to 10 km above the surface Radar reflectivityKa band reflective Radar dataAdequate Ka band radar backscatter cross-section (>-20 db) Load bearing surfaceNot dominated by dust TI 288–504, albedo low Thermal inertia >100 J m -2 s -0.5 K -1 and albedo 0.01 for load bearing bulk density

GUSEV CRATER 25 km

GUSEV CRATER From Irwin (2003), 4 th MER landing site meeting

20 km GALE CRATER

WHY HOLDEN? Alluvial fans are among the most compelling fluvial landforms on Mars. The segmentation, fan- head trenches, frontal scarps, and contributing alcoves in Holden are better developed and more complex than at any other site on Mars. No region is more heavily dissected than Margaritifer Sinus. The Late Noachian to Early Hesperian transition was arguably the most important time in Martian geologic history for fluvial activity. Sediment was delivered to this terminal basin from both inside and outside the crater. Both quiescent and dynamic deposits available.