Formation of Aromatum Chaos, Mars: Morphological Development As a Result of Volcano-Ice Interactions Harald J
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Planetary Geologic Mappers Annual Meeting
Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m. -
Thermal Studies of Martian Channels and Valleys Using Termoskan Data
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 99, NO. El, PAGES 1983-1996, JANUARY 25, 1994 Thermal studiesof Martian channelsand valleys using Termoskan data BruceH. Betts andBruce C. Murray Divisionof Geologicaland PlanetarySciences, California Institute of Technology,Pasadena The Tennoskaninstrument on boardthe Phobos '88 spacecraftacquired the highestspatial resolution thermal infraredemission data ever obtained for Mars. Included in thethermal images are 2 km/pixel,midday observations of severalmajor channel and valley systems including significant portions of Shalbatana,Ravi, A1-Qahira,and Ma'adimValles, the channelconnecting Vailes Marineris with HydraotesChaos, and channelmaterial in Eos Chasma.Tennoskan also observed small portions of thesouthern beginnings of Simud,Tiu, andAres Vailes and somechannel material in GangisChasma. Simultaneousbroadband visible reflectance data were obtainedfor all but Ma'adimVallis. We find thatmost of the channelsand valleys have higher thermal inertias than their surroundings,consistent with previousthermal studies. We show for the first time that the thermal inertia boundariesclosely match flat channelfloor boundaries.Also, butteswithin channelshave inertiassimilar to the plainssurrounding the channels,suggesting the buttesare remnants of a contiguousplains surface. Lower bounds ontypical channel thermal inertias range from 8.4 to 12.5(10 -3 cal cm-2 s-1/2 K-I) (352to 523 in SI unitsof J m-2 s-l/2K-l). Lowerbounds on inertia differences with the surrounding heavily cratered plains range from 1.1 to 3.5 (46 to 147 sr). Atmosphericand geometriceffects are not sufficientto causethe observedchannel inertia enhancements.We favornonaeolian explanations of the overall channel inertia enhancements based primarily upon the channelfloors' thermal homogeneity and the strongcorrelation of thermalboundaries with floor boundaries. However,localized, dark regions within some channels are likely aeolian in natureas reported previously. -
Formation of Mangala Valles Outflow Channel, Mars: Morphological Development and Water Discharge and Duration Estimates Harald J
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, E08003, doi:10.1029/2006JE002851, 2007 Click Here for Full Article Formation of Mangala Valles outflow channel, Mars: Morphological development and water discharge and duration estimates Harald J. Leask,1 Lionel Wilson,1 and Karl L. Mitchell1,2 Received 24 October 2006; revised 3 April 2007; accepted 24 April 2007; published 4 August 2007. [1] The morphology of features on the floor of the Mangala Valles suggests that the channel system was not bank-full for most of the duration of its formation by water being released from its source, the Mangala Fossa graben. For an estimated typical 50 m water depth, local slopes of sin a = 0.002 imply a discharge of 1 Â 107 m3 sÀ1, a water flow speed of 9msÀ1, and a subcritical Froude number of 0.7–0.8. For a range of published estimates of the volume of material eroded from the channel system this implies a duration of 17 days if the sediment carrying capacity of the 15,000 km3 of water involved had been 40% by volume. If the sediment load had been 20% by volume, the duration would have been 46 days and the water volume required would have been 40,000 km3. Implied bed erosion rates lie in the range 1to12 m/day. If the system had been bank-full during the early stages of channel development the discharge could have been up to 108 m3 sÀ1, with flow speeds of 15 m sÀ1 and a subcritical Froude number of 0.4–0.5. -
Origin of Circular Collapsed Landforms in the Chryse Region of Mars ⇑ Manuel Roda A,B, , Maarten G
Icarus 265 (2016) 70–78 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Origin of circular collapsed landforms in the Chryse region of Mars ⇑ Manuel Roda a,b, , Maarten G. Kleinhans b, Tanja E. Zegers b, Rob Govers b a Universitá degli Studi di Milano, Dipartimento di Scienze della Terra, Via Mangiagalli, 34, 20133 Milano, Italy b Universiteit Utrecht, Faculty of Geosciences, Heidelberglaan 2, 3584 CS Utrecht, The Netherlands article info abstract Article history: The quasi-circular collapsed landforms occurring in the Chryse region of Mars share similar morpholog- Received 29 June 2015 ical characteristics, such as depth of collapse and polygonally fractured floors. Here, we present a statis- Revised 20 October 2015 tical analysis of diameter, maximum and minimum depth, and amount of collapse of these features. Accepted 21 October 2015 Based on their morphometric characteristics, we find that these landforms have a common origin. In par- Available online 27 October 2015 ticular, the investigated landforms show diameter-depth correlations similar to those that impact craters of equivalent diameters exhibit. We also find that the observed amount of collapse of the collected fea- Keywords: tures is strongly correlated to their diameter. Furthermore, the linear relation between minimum filling Geological processes and pristine depth of craters, the constant ratio between collapse and the amount of filling and the frac- Ices Impact processes tured and chaotic aspect of the filling agree with melting and subsequent collapse of an ice layer below a Mars, surface sediment layer. This interpretation is consistent with a buried sub-ice lake scenario, which is a non-climatic mechanism for producing and storing abundant liquid water under martian conditions. -
New Chryse and the Provinces
New Chryse and the Provinces The city of New Chryse is actually several connected cities. The Upper City is located on a break in the crater rim, looking down past a steep rock to the Lower City. Inside the da Vinci crater rim lies the Inner City, also known as the Old City – Red Era tunnels and cave shelters, as well as several nanocomposite towers and cupolas on Mona Lys Ridge looking down on the lower parts of the city. The Lower city lies in a valley sloping down to the Harbour City, which fills a crater 20 kilometres to the East. The Harbour City crater is connected to Camiling Bay and the sea through two canyons and is very well protected from both wind and ice. South of the Lower City and Harbour City lies The Slopes, a straight slope into the sea that is covered with sprawl and slums. Mona Lys Ridge is a mixture of palatial estates surrounded by gardens, imposing official imperial buildings and towering ancient structures used by the highest ranks of the Empire. The central imperial administration and especially the Council is housed in the Deimos Needle, a diamondoid tower that together with its sibling the Phobos Needle dominate the skyline. Escalators allow swift and discreet transport down to the lower levels of the city, and can easily be defended by the police force. North of Mona Lys lies a secluded garden city for higher administrators, guild officials and lesser nobility. The Inner City is to a large extent part of Mona Lys, although most of the inhabitants of Mona Lys do not care much for the dusty old tunnels and hidden vaults – that is left to the Guild of Antiquarians who maintain and protect it. -
NEW EVIDENCE for the SHALBATANA VALLIS PALEOLAKE, MARS, from the HIGH RESOLUTION IMAGING SCIENCE EXPERIMENT (Hirise)
40th Lunar and Planetary Science Conference (2009) 1939.pdf NEW EVIDENCE FOR THE SHALBATANA VALLIS PALEOLAKE, MARS, FROM THE HIGH RESOLUTION IMAGING SCIENCE EXPERIMENT (HiRISE). G. Di Achille1, B. M. Hynek1,2, and M. L. Searls, 1Laboratory for Atmospheric and Space Physics, University of Colorado, 392 UCB, Boulder, CO 80309, United States, 2Department of Geological Sciences, University of Colorado, 392 UCB, CO 80309, United States. Introduction: A recent study has identified six possible fan-delta deposits, including a main Gilbert- type delta, at the mouths of the rare contributing chan- nels of Shalbatana Vallis, Mars, and has suggested that a former intravalley lake could have been present within one of the topographic depressions along the main valley (Fig. 1) [1]. The lake would have formed in the Hesperian (about 3.4 Ga) during the terminal hydrological activity of the valley and stabilized its main standing level at 2800 m below the Martian da- tum [1] (S1 in Fig. 1). However, no shorelines were identified on the deltas with the previous datasets, making the lacustrine interpretation questionable. Here, by using the analysis of a stereo pair of HiRISE images [2] coupled with morphometric observations from the Mars Orbiter Laser Altimeter (MOLA) topog- raphic dataset [3], we report the discovery of lake strandlines along the main Gilbert-type delta whithin Shalbatana Vallis (Fig. 2). Sub-meter scale observation of the Shalbatana Figure 1. HRSC color combination of the sedimentary de- Gilbert-type delta. The PSP_009683_1830 and posits (numbered from 1 to 6) along Shalbatana Vallis. PSP_010316_1830 HiRISE images [2] observed the central portion of Shalbatana Vallis at a resolution of of surface properties within a few hundreds of meters about 64 and 67 cm/pixel, respectively. -
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, -
Aromatum Chaos: Heating Up, Melting Ice, and Letting It Flow – a Preliminary Analysis
46th Lunar and Planetary Science Conference (2015) 2999.pdf AROMATUM CHAOS: HEATING UP, MELTING ICE, AND LETTING IT FLOW – A PRELIMINARY ANALYSIS. K. L. Craft,1 R. P. Lowell2, and S. Potter-McIntyre3 1Johns Hopkins University Applied Physics Laboratory (11100 Johns Hopkins Rd., Laurel, MD 20723, [email protected]), 2Virginia Tech, 4044 Derring Hall, Blacksburg, VA, 3Southern Illinois University, Carbondale, IL 62901. Introduction: Evidence of magmatic activity on subsequent fluid flow through dike-driven Mars is abundant and has been occurring from the hydrothermal system at Aromatum Chaos, we model Noachian period to geologically recent years [1]. Many the system as shown below in Figure 2 using boundary features also exist on the surface that indicate this layer theory, as described by [7] and previously magmatic activity interacted with water in both its applied by [6] at Athabasca Valles. We build on the liquid and solid forms [e.g.1-3]. Out of the fire and ice, previous work by also considering convection in an hydrothermal systems are born that circulate overlying permafrost melt layer through a scale chemicals, fluids and heat. The combination of water, analysis. Our models attempt to determine if such a heat and energy make for ideal habitable zones. As system could bring adequate water to the surface to form the Ravi Vallis outflow channels. A dike of well, on Earth, mid-ocean ridge hydrothermal systems about 1200°C heats the system from the side, causing a have been suggested as a possible location for the first wall temperature of about 600°C between the magma terrestrial life [4]. -
Erosive Flood Events on the Surface of Mars: Application to Mangala and Athabasca Valles Alistair Simon Bargery, Lionel Wilson
Erosive flood events on the surface of Mars: application to Mangala and Athabasca Valles Alistair Simon Bargery, Lionel Wilson To cite this version: Alistair Simon Bargery, Lionel Wilson. Erosive flood events on the surface of Mars: application to Mangala and Athabasca Valles. Icarus, Elsevier, 2011, 212 (2), pp.520. 10.1016/j.icarus.2011.01.001. hal-00734590 HAL Id: hal-00734590 https://hal.archives-ouvertes.fr/hal-00734590 Submitted on 24 Sep 2012 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. Accepted Manuscript Erosive flood events on the surface of Mars: application to Mangala and Atha‐ basca Valles Alistair Simon Bargery, Lionel Wilson PII: S0019-1035(11)00002-9 DOI: 10.1016/j.icarus.2011.01.001 Reference: YICAR 9680 To appear in: Icarus Received Date: 20 June 2010 Revised Date: 28 December 2010 Accepted Date: 3 January 2011 Please cite this article as: Bargery, A.S., Wilson, L., Erosive flood events on the surface of Mars: application to Mangala and Athabasca Valles, Icarus (2011), doi: 10.1016/j.icarus.2011.01.001 This is a PDF file of an unedited manuscript that has been accepted for publication. -
Paleoflooding in the Solar System: Comparison Among Mechanisms For
Paleoflooding in the Solar System: comparison among mechanisms for flood generation on Earth, Mars, and Titan Devon Burr Earth and Planetary Sciences Department EPS 306 University of Tennessee Knoxville 1412 Circle Dr. Knoxville TN 39776-1410 USA [email protected] ABSTRACT Conditions allow surficial liquid flow on three bodies in the Solar System, Earth, Mars, and Titan. Evidence for surficial liquid flood flow has been observed on Earth and Mars. The mechanisms for generating flood flow vary according to the surficial conditions on each body. The most common flood-generating mechanism on Earth is wide-spread glaciation, which requires an atmospheric cycle of a volatile that can assume the solid phase. Volcanism is also a prevalent cause for terrestrial flooding, which other mechanisms producing smaller, though more frequent, floods. On Mars, the mechanism for flood generation has changed over the planet’s history. Surface storage of floodwater early in Mars’ history gave way to subsurface storage as Mars’ climate deteriorated. As on Earth, Mars’ flooding is an effect of the ability of the operative volatile to assume the solid phase, although on Mars, this has occurred in the subsurface. According to this paradigm, Titan conditions preclude extreme flooding because the operative volatile, which is methane, cannot assume the solid phase. Mechanisms that produce smaller but more frequent floods on Earth, namely extreme precipitation events, are likely the most important flood generators on Titan. 1. Introduction The historical flow of paleoflood science has risen and fallen largely in concert with prevailing scientific paradigms (Baker 1998). The paradigm in the 17 th century was catastrophism, the idea that geology is the product of sudden, short, violent events. -
Timing of Fluvial Activity in the Xanthe Terra Region of Mars: Implications for Hypanis Delta, a Potential Landing Site for Mars2020
47th Lunar and Planetary Science Conference (2016) 2196.pdf TIMING OF FLUVIAL ACTIVITY IN THE XANTHE TERRA REGION OF MARS: IMPLICATIONS FOR HYPANIS DELTA, A POTENTIAL LANDING SITE FOR MARS2020. S. Eckes1, N.H. Warner1, S. Gup- ta2, M. O’Shea1, J. Smith1, A. Werynski1, 1Department of Geological Sciences, SUNY Geneseo, 1 College Circle, Geneseo, NY 14454; 2Imperial College London, South Kensington Campus, Earth Science and Engineering, Lon- don, SW7 2AZ, UK. [email protected] & [email protected] Introduction: The Xanthe Terra region of Mars > 200 m diameter craters rest solely on top of these exhibits multiple fluvial networks that are of interest ejecta blankets. It is possible, given the thickness of the for future exploration. The timing of these channels is ejecta blankets for (order of) 10 km-size craters and poorly constrained and it’s not clear whether they given depth/diameter relationships of craters of this formed at the same time or spanned a broader period of size [6,7], that some craters may poke through the ejec- history [1,2,3]. Furthermore, sedimentary fans that are ta from the highland terrain beneath. This scenario sourced by some of the channels are currently under would provide an overestimate of the formation age of consideration as landing sites for Mars2020. It is there- the larger crater using crater statistics. fore critical to understand their timing within the To better understand and resolve this issue, we chronostratigraphic context of Mars. Current estimates, constrained a mean thickness for each ejecta blanket in based on crater counts from the fans, places the fluvial our count analysis using a 100 m High Resolution Ste- activity within the Hesperian to Early Amazonian reo Camera digital elevation model (DEM). -
Geologic Map of the Source Region of Shalbatana Vallis, Mars
Geologic Map of the Source Region of Shalbatana Vallis, Mars Dan Berman, Cathy Weitz, Alexis Rodriguez, and David Crown Planetary Mappers Meeting Flagstaff, AZ June 12-13, 2017 Introduction •We are currently producing a 1:500,000-scale USGS geologic map of MTM quadrangles 00042 and 00047 in the Xanthe Terra region of Mars (2.5°S - 2.5°N, 310° - 320°E). The map region has been extensively modified by outflow channels and chaotic terrains and contains cratered plains deformed by subsidence. Mapping is being conducted on a THEMIS IR daytime base mosaic, with CTX and HiRISE images as supplements where available. •The overarching goal of this project is to develop an understanding of how regionally integrated hydrologic systems have been affected by (1) impact crater formation, (2) melting of subsurface ice leading to the generation of subsurface cavity space and then subsidence, and (3) erosional and depositional flooding events of various types and ages. Chryse Planitia Kasei Vallis Simud Vallis Tiu Maja Vallis Vallis Chryse Chaos Ares Vallis Shalbatana Xanthe Vallis Terra Hydraotes Chaos Ganges Chasma Description of Map Units Plains Units •cratered plains 1 – smooth to mottled, heavily cratered plains marked by secondary chains, wrinkle ridges, and zones of incipient collapse. Ejecta of many large craters entirely or partly eroded •cratered plains 2 – similar to cratered plains 1, with dark signature in THEMIS day IR (bright in night IR) and some knobs Crater Units •crater material – crater ejecta, rim, and floor materials •crater fill material