DOCSLIB.ORG

Mars Pathfinder Landing Site Workshop

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Mars Pathfinder Landing Site Workshop NASA-CR-196745 MARS PATHFINDER LANDING SITE WORKSHOP (NASA-CR-196745) MARS PATHFINDER N95-14276 LANDING SITE WORKSHOP Abstracts --THR U-- Only (Lunar and Planetary Inst.) N95-16208 57 P Unclas G3/91 0020918 LPI Technical Report Number 94-04 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1 113 LPI/TR--94-04 MARS PATHFINDER LANDING SITE WORKSHOP Edited by M. Golombek Held at Houston, Texas April 18-19,1994 Sponsored by Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1 1 13 LPI Technical Report Number 94-04 LPUTR--94-04 I- Compiled in 1994 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the University 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 Golombek M..ed. (1994) Mars Parhfinder Landing Sire Workshop. LPI Tech. Rpt. 94-04, Lunar and Planetary Institute, Houston. 49 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058- 1 I 13 Mail order requesrors will be invoiced for /he cost of shipping and handling. LPI Technical Report 94-04 iii Preface The Mars Pathfinder Project is an approved Discovery-class mission that will place a lander and rover on the surface of the Red Planet in July 1997. On April 18-19,1994, a Mars Pathfinder Landing Site Workshop was held at the Lunar and Planetary Institute in Houston, Texas, under the auspices of the Jet Propulsion Laboratory Mars Pathfinder Project and the Lunar and Plan- etary Institute. The workshop was designed to allow the Mars scientific community to provide input as to where to land Pathfinder on Mars. The workshop was attended by over 60 people from around the United States and from Europe. Over 20 landing sites were proposed at the workshop, and the scientific questions and problems concerning each were addressed. The workshop and the discussion that occurred during and afterward have signifi- cantly improved our ability to select a scientifically exciting but safe landing site on Mars. LPI Technical Report 94-04 Y ogram Monday morning, April 18,1994 Workshop Introduction and Overview M. Golombek* HOW WILL WE GET THERE? MISSION INTRODUCTION Chair: M. Golombek Project Status A. Spear* Mission Design and Flight System R. Cook* Rover and Surface Scenarios W.Dias* WHAT MEASUREMENTS WILL WE MAKE AFTER WE GET THERE? INSTRUMENT DESCRIPTIONS Chair: J. Wellman Imager for Mars Pathfinder (IMP) P. Smith* Surface Science Capabilities from IMP Spectral Imaging R. Singer* Alpha Proton X-Ray Spectrometer R. Rieder*, H. Wanke, and T. Economou Atmospheric Structure and Meteorology Instrument for Mars Pathfinder A. SeifP vi Mars Pathfinder Workshop Monday afternoon, April 18,1994 WHY SHOULD WE GO TO THAT SITE? GENERAL LANDING SITE PERSPECTIVES Chair: D. Des Marais A Perspective of Landing-Site Selection H. J. Moore* Strategy for Selecting Mars Pathfinder Landing Sites R. Greeley* and R. Kuzmin Exobiology Site Priorities for Mars Pathfinder J. Farmer* and D. DesMarais Landing Site Considerations for Atmosphere Structure and Meteorology A. SeifP, R. Haberle, and J. Murphy WHERE ARE WE? WHAT WILL IT LOOK LIKE? HOW SAFE WILL IT BE? WHAT WILL THE WEATHER BE? WHAT WAS THE WEATHER LIKE? Chair: R. Greeley Observations by the Mars '94 Orbiter and Possible Correlations with Mars Pathfinder H. U. Keller* Implications of High-Spatial-Resolution Thermal Infrared (Termoskan)Data for Mars Landing Site Selection B. H. Betts* Goldstone Radar Contributions to Mars Pathfinder Landing Safety M. A. Slade* and R. F. Jurgens Meteorological Observations of Synoptic Disturbances: Sensitivity to Latitude J. Barnes* Mars Pathfinder Meteorological Observations on the Basis of Results of an Atmospheric Global Circulation Model F. Forget*, F. Hourdin, and 0. Talagrand Climatological Targetsfor Mars Pathfinder A. P. Zent* LPI Technical Report 94-04 Vii I Monday evening, April 18,1994 POSTER DISCUSSION AND RECEPTION Potential Landing Sites for Mars Pathfinder R. Kuzmin, R. Landheim, and R. Greeley Physical Properties (Particle Size, Rock Abundance)from Thermal Infrared Remote Observations: Implications for Mars Landing Sites P. R. Christensen and K. S. Edgett Tuesday morning, April 19,1994 WHAT LONGITUDE ARE WE GOING TO? (Le., WHERE DO WE TARGET THE ROCKET?) WHAT WILL WE LEARN AFTER WE GET THERE? 2SoW-55"W Longitude Chair: J. Plescia Rationale for a Mars Pathfinder Mission to Chryse Planitia and the Viking I Lander R. A. Craddock* Chryse Planitia as a Mars Pathfinder Landing Site: The Imperative of Building on Previous Ground Truth L. S. Crumpler* Maja Valles and the Chryse Outflow Complex Sites J. W. Rice* A Highland Sample Strategy for Pathfinder R. A. De Hon* Meles Chasma: A Mars Pathfinder View of Valles Marineris A. H. Treiman* and S. Murchie 145"W-200" W Longitude Chair: R. Singer Scientific Rationale for Selecting Northern Eumenides Dorsum (9"-11 "N Latitude, I59"-162" Longitude) as a Potential Mars Pathfinder Landing Site T. 3. Parker* Mars Pathfinder and the Exploration of Southern Amazonis Planitia N. G. Barlow* viii Mars Pathfinder Workshop Pathfinder Landing Sites at Candidate SNC Impact Ejection Sites M. P. Golombek* Marta Valles Channel System in the Cerberus Rupes Region (16ON, 177OW) J. W. Rice* Cerberus Plains: A Most Excellent Pathfinder Landing Site J. B. Plescia* Tuesday afternoon, April 19, I994 14S0W-2OO0W Longitude - continued A Mars Pathfinder Landing on a Recently Drained Ephemeral Sea: Cerberus Plains G. R. Brakenridge" Opportunity to Sample Something Different: The Dark, Unweathered, Mafic Sands of Cerberus and the Pathfinder 1997 Mars Landing K. S. Edgett*, R. B. Singer, and P. E. Geissler Tartarus Colles: A Sampling of the Martian Highlands S. Murchie* and A. Treiman 220°W-2800W Longitude Chair: A. Treiman Sampling Elysium Lavas (13"N, 203"W) C. C. Allen* Rationale for Isidis Planitia as a Back-up Landing Site for the Mars Pathfinder Mission R. A. Craddock* Scientific Rationale for Selecting Northwest Isidis Planitia (14O-17ON Latitude, 278"-281 O Longitude) as a Potential Mars Pathfinder Landing Site T. J. Parker* and J. W. Rice Discussion LPI Technical Report 94-04 iX Contents MissionDescription ................................................................................................................................ 1 . Summary of Technical Sessions .............................................................................................................. 5 .. Abstracts ............................................................................................................................................... 15 List of Workshop Participants .............................................................................................................. 45 LPI Technical Reporr 94-04 1 .e .e ,/ I 7 /7,& -- *, Mission Description The Mars Pathfinder Project received a new start in October to navigational uncertainties during cruise and atmospheric 1993 as the next mission in NASA's long-term Mars explora- entry. All parts of this landing ellipse must satisfy the specified tion progmn. 'Ihe mission involves landing a single vehicle on latitude and elevation constraints. the surface of Mars in 1997.The project is required to be low cost Landing occurs just after Earth rise and approximately four ($1 50M development cost cap), have a fast schedule (less than hours before sunrise. The highest-priority activities on the three years' development period), and achieve a set of signifi- landing sol are to achieve an upright landed configuration, cant but focused engineering, science, and technology objec- return the recorded entry science and engineering data, estab- tives. The primary objective is to demonstrate lowcost cruise, lish a high-rate telecommunications link, acquire and return a entry, descent, and landing systems required to place a payload panoramic image of the surrounding terrain, and deploy the on the martian surface in a safe, operational configuration. rover. Surface operations for the remainder of the 30-sol pri- Additional objectives intlude the deployment and operation of mary mission are focused on extensive use of the rover and various science instruments and a microrover. Pathfinder paves science instruments. the way for a cost-effective implementation of future Mars lander missions as part of a comprehensive Mars exploration SPACECR4FT DESCRIPTION program. Pathfinder will be launched on a Type 1 Earth-Mars transfer The Pathfinder flight system consists of three major ele- trajectory on a McDonnell Douglas Delta I1 7925 launch ve- ments: the cruise stage, the deceleration subsystems, and the hicle. Current planning assumes a 30-day launch period ex- lander (containing the rover and science instruments). The tendingfromDecember5,19%, toJanuary3.1997,withafixed current spacecraft launch mass is approximately 710 kg, includ- Mars arrival date of July 4, 1997. ing 25 kg of payload (science instruments, rover, and rover The 6-7-month cruise phase is a relatively quiescent period support equipment). in which spacecraft activities are minimized. The primary The cruise stage is used to perform launch vehicle separa- activities include periodic
Load more

Recommended publications
  • 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]
  • Numerical Modeling of Magnetic Capture of Martian Atmospheric Dust ______
    ____________________________________________________________________________ Numerical Modeling of Magnetic Capture of Martian Atmospheric Dust __________________________________________________________________________ Kjartan Kinch Mars Simulation Laboratory Institute of Physics and Astronomy Aarhus University, Denmark Ph.D. Thesis Revised Edition March 2005 III Table of Contents Table of Contents .................................................................................. III List of Publications...............................................................................VII Preface.................................................................................................... IX 1. Introduction.........................................................................................1 1.1. The Mars Exploration Rover mission .................................................................1 1.2. Dust in the Martian Atmosphere .........................................................................2 1.3. Magnetic Properties Experiments .......................................................................3 1.4. The Present Work................................................................................................5 1.4.1. Motivation and Method......................................................................................5 1.4.2. Structure of the Thesis .......................................................................................5 2. The Planet Mars..................................................................................7
    [Show full text]
  • Vertical Distribution of Dust in the Martian Atmosphere During Northern Spring and Summer: High‐Altitude Tropical Dust Maximum at Northern Summer Solstice N
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 116, E01007, doi:10.1029/2010JE003692, 2011 Vertical distribution of dust in the Martian atmosphere during northern spring and summer: High‐altitude tropical dust maximum at northern summer solstice N. G. Heavens,1,2 M. I. Richardson,3 A. Kleinböhl,4 D. M. Kass,4 D. J. McCleese,4 W. Abdou,4 J. L. Benson,4 J. T. Schofield,4 J. H. Shirley,4 and P. M. Wolkenberg4 Received 7 July 2010; revised 2 November 2010; accepted 12 November 2010; published 20 January 2011. [1] The vertical distribution of dust in Mars’ atmosphere is a critical unknown in the simulation of its general circulation and a source of insight into the lifting and transport of dust. Zonal average vertical profiles of dust opacity retrieved by Mars Climate Sounder show that the vertical dust distribution is mostly consistent with Mars general circulation model (GCM) simulations in southern spring and summer but not in northern spring and summer. Unlike the GCM simulations, the mass mixing ratio of dust has a maximum at 15– 25 km over the tropics during much of northern spring and summer: the high‐altitude tropical dust maximum (HATDM). The HATDM has significant and characteristic longitudinal variability, which it maintains for time scales on the order of or greater than those on which advection, sedimentation, and vertical eddy diffusion would act to eliminate both the longitudinal and vertical inhomogeneity of the distribution. While outflow from dust storms is able to produce enriched layers of dust at altitudes much greater than 25 km, tropical dust storm activity during the period in which the HATDM occurs is likely too rare to support the HATDM.
    [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]
  • Ca Li for Ni a Insc Itu Te of Techno Logy Voillme LX, Nllmber 3, I 997
    Ca li for ni a Insc itu te of Techno logy SC I EN CE Voillme LX, Nllmber 3, I 997 IN THIS ISSUE Water and Ancient Mars Geology Under the Antarctic Ocean Arsenic and the L.A . Aqueduct Top: Every explorer wants to see what's on the other side of the next hill. When Sojourner, the Mars Path­ finder's rover, peered over a nearby crest on Sol (Mar- tian day) 76, it saw what appear to be sand dunes. If the stuff really is sand (a question that is still being debated), it implies the likely long-term prese.nce of liquid water-the most plausible agent for creating sand-sized grains. The Twin Peaks are on the horizon on the right; the "Big" Crater is on the left. Bottom: The rover took this picture of the lander, nesting comfortably in its deflated air bags, on Sol 33. You can see the for­ ward ramp, which sticks straight out like a diving board instead of bending down to touch the Martian surface (the rover drove off the rear ramp). And if you think you see E.T.'s face, you're not far wrong­ Pathfinder's camera has two "eyes" spaced 15 cen­ timeters apart for stereo vision. For a look at what else Pathfinder has seen, turn to page 8. " N GIN E E R I N G & C 1 ENe E Ca li for n ia Instit u te o f Tec h no logy 2 Random Wa lk 8 Pathfinder's Fi n ds - by Dougla s L.
    [Show full text]
  • Mineralogy of the Martian Surface
    EA42CH14-Ehlmann ARI 30 April 2014 7:21 Mineralogy of the Martian Surface Bethany L. Ehlmann1,2 and Christopher S. Edwards1 1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125; email: [email protected], [email protected] 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 Annu. Rev. Earth Planet. Sci. 2014. 42:291–315 Keywords First published online as a Review in Advance on Mars, composition, mineralogy, infrared spectroscopy, igneous processes, February 21, 2014 aqueous alteration The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: The past fifteen years of orbital infrared spectroscopy and in situ exploration 10.1146/annurev-earth-060313-055024 have led to a new understanding of the composition and history of Mars. Copyright c 2014 by Annual Reviews. Globally, Mars has a basaltic upper crust with regionally variable quanti- by California Institute of Technology on 06/09/14. For personal use only. All rights reserved ties of plagioclase, pyroxene, and olivine associated with distinctive terrains. Enrichments in olivine (>20%) are found around the largest basins and Annu. Rev. Earth Planet. Sci. 2014.42:291-315. Downloaded from www.annualreviews.org within late Noachian–early Hesperian lavas. Alkali volcanics are also locally present, pointing to regional differences in igneous processes. Many ma- terials from ancient Mars bear the mineralogic fingerprints of interaction with water. Clay minerals, found in exposures of Noachian crust across the globe, preserve widespread evidence for early weathering, hydrothermal, and diagenetic aqueous environments. Noachian and Hesperian sediments include paleolake deposits with clays, carbonates, sulfates, and chlorides that are more localized in extent.
    [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]
  • Planet Mars III 28 March- 2 April 2010 POSTERS: ABSTRACT BOOK
    Planet Mars III 28 March- 2 April 2010 POSTERS: ABSTRACT BOOK Recent Science Results from VMC on Mars Express Jonathan Schulster1, Hannes Griebel2, Thomas Ormston2 & Michel Denis3 1 VCS Space Engineering GmbH (Scisys), R.Bosch-Str.7, D-64293 Darmstadt, Germany 2 Vega Deutschland Gmbh & Co. KG, Europaplatz 5, D-64293 Darmstadt, Germany 3 Mars Express Spacecraft Operations Manager, OPS-OPM, ESA-ESOC, R.Bosch-Str 5, D-64293, Darmstadt, Germany. Mars Express carries a small Visual Monitoring Camera (VMC), originally to provide visual telemetry of the Beagle-2 probe deployment, successfully release on 19-December-2003. The VMC comprises a small CMOS optical camera, fitted with a Bayer pattern filter for colour imaging. The camera produces a 640x480 pixel array of 8-bit intensity samples which are recoded on ground to a standard digital image format. The camera has a basic command interface with almost all operations being performed at a hardware level, not featuring advanced features such as patchable software or full data bus integration as found on other instruments. In 2007 a test campaign was initiated to study the possibility of using VMC to produce full disc images of Mars for outreach purposes. An extensive test campaign to verify the camera’s capabilities in-flight was followed by tuning of optimal parameters for Mars imaging. Several thousand images of both full- and partial disc have been taken and made immediately publicly available via a web blog. Due to restrictive operational constraints the camera cannot be used when any other instrument is on. Most imaging opportunities are therefore restricted to a 1 hour period following each spacecraft maintenance window, shortly after orbit apocenter.
    [Show full text]
  • Inferences of Martian Atmospheric Dust and Water Ice Content Derived from Radiative Transfer Models of Passive Msl Observations by Mastcam
    44th Lunar and Planetary Science Conference (2013) 1288.pdf INFERENCES OF MARTIAN ATMOSPHERIC DUST AND WATER ICE CONTENT DERIVED FROM RADIATIVE TRANSFER MODELS OF PASSIVE MSL OBSERVATIONS BY MASTCAM. E. M. McCul- lough1, J. E. Moores 1,2, R. Francis1, and the MSL Science Team. 1Centre for Planetary Science and Exploration (The University of Western Ontario, London, ON, Canada, [email protected]), 2Now at: Centre for Research in Earth and Space Sciences (CRESS, York University, Toronto, ON, Canada). Introduction: While the Mars Science Laboratory cameras [3]. The 440 nm and 750 nm combination of (MSL) Spacecraft was not designed primarily as a ve- wavelengths was chosen because this ratio is the least hicle from which to study the martian atmosphere, the ambiguous for distinguishing ice from dust. recent landing of MSL's rover Curiosity has provided The MastCam's left and right cameras can be used opportunities to extend the science return of the exist- simultaneously to image the sky, with a 440 nm blue ing instrument complement to include observations of filter on the right camera and a 750 nm red filter on the atmospheric water ice and dust. left. Alternately, sequential images taken in both wave- The participating science project “Observations of lengths with a single camera (typically MastCam Left), Water Ice and Winds from the MSL Rover” [1], in- can be used. The latter is the simplest case with which cluded proposed atmospheric measurements using sev- to begin as many camera-specific parameters will be eral MSL imagers. To date, several such data products identical for the pair of images.
    [Show full text]
  • Rockyfor3d (V5.2) Revealed
    Rockyfor3D (v5.2) revealed Transparent description of the complete 3D rockfall model Publication information Author Dr. Luuk K.A. Dorren (Bern University of Applied Sciences, CH) Contributors to model development Dr. Frédéric Berger (Irstea Grenoble, FR) Dr. Franck Bourrier (Irstea Grenoble, FR) Prof. Dr. Willem Bouten (Universiteit van Amsterdam, NL) Dr. Luuk K.A. Dorren (Bern University of Applied Sciences, CH) Mathilde Gallouet (UJF Grenoble, FR) Roderick Kühne (Universität Bern, CH) Uif S. Putters (Universiteit van Amsterdam, NL) Dr. Bahjat Safadi (LIG Grenoble, FR) Dr. Harry C. Seijmonsbergen (Universiteit van Amsterdam, NL) Dr. Sanneke van Asselen (Vrije Universiteit Amsterdam, NL) Dr. Mark J. van Wijk (Wageningen University, NL) Prof. Dr. Jasper Vrugt (University of California – Irvine, US) Nicolas Zuanon (A2 Photonic Sensors, FR) Publisher Int. ecorisQ Association Geneva Switzerland Citation Dorren L.K.A., 2016. Rockyfor3D (v5.2) revealed – Transparent description of the complete 3D rockfall model. ecorisQ paper (www.ecorisq.org): 32 p. © ecorisQ 2016 Date: 30.03.2016 Reprinting is allowed, except for commercial use, if citing the source. Thanks go to the following colleagues for valuable suggestions Dr. Ulrik Domaas (NGI, NO), Dr. Oliver Jancke (Irstea Grenoble, FR), Dr. Jean-Bruno Pasquier (Géoval, CH) Content 1 Introduction ........................................................................................................ 1 2 Model input and quick start ...............................................................................
    [Show full text]
  • Global Geometric Properties of Martian Impact Craters: a Preliminary Assessment Using Mars Orbiter Laser Altimeter (Mola)
    GLOBAL GEOMETRIC PROPERTIES OF MARTIAN IMPACT CRATERS: A PRELIMINARY ASSESSMENT USING MARS ORBITER LASER ALTIMETER (MOLA). J. B. Garvin1, S. E. H. Sakimoto2, C. Schnetzler3, and J. J. Frawley4, 1(NASAÕs GSFC, Code 921, Greenbelt, MD 20771 USA; [email protected]), 2(USRA at NASAÕs GSFC, Code 921, Greenbelt, MD 20771), 3(SSAI at NASAÕs GSFC) 4(H-STX and Herring Bay Geophysics at NASAÕs GSFC). Introduction: Impact craters on Mars have been ÒshapeÓ (n), central peak height, diameter D, volume, used to provide fundamental insights into the proper- shape, and many others. In this report, we treat the ties of the martian crust, the role of volatiles, the rela- crater depth versus diameter relationship, the crater rim tive age of the surface, and on the physics of impact height vs. diameter pattern, the statistics of ejecta cratering in the Solar System [1,2,6]. Before the three- thickness and its spatial distribution, and cavity geo- dimensional information provided by the Mars Orbiter metric properties, including interior deposit geometry. Laser Altimeter (MOLA) instrument which is currently Crater depth vs. Diameter: Using MOLA topog- operating in Mars orbit aboard the Mars Global Sur- raphic profile data, we have computed the total depth veyor (MGS), impact features were characterized mor- (from rim crest to lowest point on crater cavity floor) phologically using orbital images from Mariner 9 and and true depth (i.e., from pre-impact surface to mean Viking. Fresh-appearing craters were identified and crater floor level) for over 1300 craters. When we exam- measurements of their geometric properties were de- ine the correlation of depth d against diameter D, a rived from various image-based methods [3,6].
    [Show full text]
  • Tuesday, March 22, 2016 [T328] POSTER SESSION I: MARTIAN GULLIES, SLOPE STREAKS, and MASS WASTING 6:00 P.M
    47th Lunar and Planetary Science Conference (2016) sess328.pdf Tuesday, March 22, 2016 [T328] POSTER SESSION I: MARTIAN GULLIES, SLOPE STREAKS, AND MASS WASTING 6:00 p.m. Town Center Exhibit Area Glines N. H. Gulick V. C. Freeman P. M. Rodriguez J. A. P. Hargitai H. POSTER LOCATION #437 Indications of Meltwater-Driven Gully Formation in Moni Crater, Mars [#2464] Glacial and post-glacial processes have significantly modified the landscape of Moni Crater, Mars, where meltwater is likely the key gully formation mechanism. Conway S. J. Harrison T. N. Lewis S. R. Soare R. J. Balme M. R. et al. POSTER LOCATION #438 Martian Gully Orientation and Slope Used to Test Meltwater and Carbon Dioxide Hypotheses [#1973] We use re-analysis of the global gully-data and 1D climate models to assess the CO2 and meltwater hypotheses for gully-formation. Puga F. Pina P. POSTER LOCATION #439 13 Years of Temporal Fading Quantification in Dark Slope Streaks from Lycus Sulci [#2076] We present a tool to measure the full pixel analyses albedo contrast between slope streaks and their neighborhood regions. Sarkar R. Singh P. Ganesh I. POSTER LOCATION #440 Origin of Mass Wasting Features in Juventae Chasma, Mars [#1876] This contribution reports mass- wasting features originating from the walls of Juventae Chasma. Debniak K. T. Kromuszczynska O. POSTER LOCATION #441 Geomorphological Characteristics of Mass-Wasting Features in Ius Chasma, Valles Marineris, Mars [#1890] Mass-wasting features mapped in Ius Chasma have been assigned to six major categories. The results present a new classification of large landslide deposits. Pietrek A.
    [Show full text]