Global Distributions of Mafic Mineral Abundances on Mars Riu L., Poulet F., Bibring J
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Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: Implications for Fluvial, Glacial, and Glaciofluvial Activity Frances E.G
Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity Frances E.G. Butcher, Matthew Balme, Susan Conway, Colman Gallagher, Neil Arnold, Robert Storrar, Stephen Lewis, Axel Hagermann, Joel Davis To cite this version: Frances E.G. Butcher, Matthew Balme, Susan Conway, Colman Gallagher, Neil Arnold, et al.. Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. Icarus, Elsevier, 2021, 10.1016/j.icarus.2020.114131. hal-02958862 HAL Id: hal-02958862 https://hal.archives-ouvertes.fr/hal-02958862 Submitted on 6 Oct 2020 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 Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: 2 Implications for Fluvial, Glacial, and Glaciofluvial Activity. 3 Frances E. G. Butcher1,2, Matthew R. Balme1, Susan J. Conway3, Colman Gallagher4,5, Neil 4 S. Arnold6, Robert D. Storrar7, Stephen R. Lewis1, Axel Hagermann8, Joel M. Davis9. 5 1. School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6 6AA, UK. 7 2. Current address: Department of Geography, The University of Sheffield, Sheffield, S10 8 2TN, UK ([email protected]). -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: Implications for Fluvial, Glacial, and Glaciofluvial Activity
This is a repository copy of Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/166644/ Version: Published Version Article: Butcher, F.E.G. orcid.org/0000-0002-5392-7286, Balme, M.R., Conway, S.J. et al. (6 more authors) (2021) Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. Icarus, 357. 114131. ISSN 0019-1035 https://doi.org/10.1016/j.icarus.2020.114131 Reuse This article is distributed under the terms of the Creative Commons Attribution (CC BY) licence. This licence allows you to distribute, remix, tweak, and build upon the work, even commercially, as long as you credit the authors for the original work. More information and the full terms of the licence here: https://creativecommons.org/licenses/ Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ Journal Pre-proof Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity Frances E.G. Butcher, Matthew R. Balme, Susan J. Conway, Colman Gallagher, Neil S. Arnold, Robert D. Storrar, Stephen R. Lewis, Axel Hagermann, Joel M. Davis PII: S0019-1035(20)30473-5 DOI: https://doi.org/10.1016/j.icarus.2020.114131 Reference: YICAR 114131 To appear in: Icarus Received date: 2 June 2020 Revised date: 19 August 2020 Accepted date: 28 September 2020 Please cite this article as: F.E.G. -
Workshop on Mars Telescopic Observations
WORKSHCPON MARS TELESCOPIC OBSERVATIONS 90' 180'-;~~~~~~------------------..~~------------~~----..~o~,· 270' LPI Technical Report Number 95-04 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPIITR--95-04 WORKSHOP ON MARS TELESCOPIC OBSERVATIONS Edited by J. F. Bell III and J. E. Moersch Held at Cornell University, Ithaca, New York August 14-15, 1995 Sponsored by Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 95-04 LPIITR--95-04 Compiled in 1995 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities 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 Bell J. F.III and Moersch J. E., eds. (1995) Workshop on Mars Telescopic Observations. LPI Tech. Rpt. 95-04, Lunar and Planetary Institute, Houston. 33 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Mail order requestors will be invoiced for the cost ofshipping and handling. Cover: Orbits of Mars (outer ellipse) and Earth (inner ellipse) showing oppositions of the planet from 1954to 1999. From C. Aammarion (1954) The Flammarion Book ofAstronomy, Simon and Schuster, New York. LPl Technical Report 95-04 iii Introduction The Mars Telescopic Observations Workshop, held August 14-15, 1995, at Cornell University in Ithaca, New York, was organized and planned with two primary goals in mind: The first goal was to facilitate discussions among and between amateur and professional observers and to create a workshop environment fostering collaborations and comparisons within the Mars ob serving community. -
Global Spectral Classification of Martian Low-Albedo Regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) Data A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, E02004, doi:10.1029/2006JE002726, 2007 Global spectral classification of Martian low-albedo regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) data A. Deanne Rogers,1 Joshua L. Bandfield,2 and Philip R. Christensen2 Received 4 April 2006; revised 12 August 2006; accepted 13 September 2006; published 14 February 2007. [1] Martian low-albedo surfaces (defined here as surfaces with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) albedo values 0.15) were reexamined for regional variations in spectral response. Low-albedo regions exhibit spatially coherent variations in spectral character, which in this work are grouped into 11 representative spectral shapes. The use of these spectral shapes in modeling global surface emissivity results in refined distributions of previously determined global spectral unit types (Surface Types 1 and 2). Pure Type 2 surfaces are less extensive than previously thought, and are mostly confined to the northern lowlands. Regional-scale spectral variations are present within areas previously mapped as Surface Type 1 or as a mixture of the two surface types, suggesting variations in mineral abundance among basaltic units. For example, Syrtis Major, which was the Surface Type 1 type locality, is spectrally distinct from terrains that were also previously mapped as Type 1. A spectral difference also exists between southern and northern Acidalia Planitia, which may be due in part to a small amount of dust cover in southern Acidalia. Groups of these spectral shapes can be averaged to produce spectra that are similar to Surface Types 1 and 2, indicating that the originally derived surface types are representative of the average of all low-albedo regions. -
Dark Dunes on Mars
CHAPTER II: PLANET MARS – THE BACKGROUND Like Earth, its neighbour planet, Mars, is a terrestrial planet with a solid surface, an atmosphere, two ice-covered pole caps, and not one but two moons (Phobos and Deimos). Some differences, such as a greater distance to the sun, a smaller diameter, a thinner atmosphere, and the longer duration of a year distinguish Mars from the Earth, not to forget the absence of life…so far. Nevertheless, there are many correlations between terrestrial and Martian geological and geomorphological processes, permitting researchers to apply knowledge from terrestrial studies more or less directly to Mars. However, a closer look reveals that the dissimilarities, though few, can make fundamental differences in process background and development. The following chapter provides a brief but necessary insight into the geological and physical background of this planet, imparting to the reader some fundamental knowledge about Mars, which is useful for understanding this work. Fig. 1 presents an impression of Mars viewed from space. Figure 1: The planet Mars: a global view (Viking 1 Orbiter mosaic [NASA]). Chapter II Planet Mars – The Background 5 Table 1 provides a summary of some major astronomical and physical parameters of Mars, giving the reader an impression of the extent to which they differ from terrestrial values. Table 1: Parameters of Mars [Kieffer et al., 1992a]. Property Dimension Orbit 227 940 000 km (1.52 AU) mean distance to the Sun Diameter 6794 km Mass 6.4185 * 1023 kg 3 Mean density ~3.933 g/cm Obliquity -
Mars Water Posters
Lunar and Planetary Science XXXVII (2006) sess608.pdf Thursday, March 16, 2006 POSTER SESSION II: MARS FLOWING AND STANDING WATER 7:00 p.m. Fitness Center Bargery A. S. Wilson L. Modelling Water Flow with Bedload on the Surface of Mars [#1218] We theorise the thermodynamical effects of entrainment of eroded cold rock and ice on proposed aqueous flow on the surface of Mars, at temperatures well below the triple point, with an upper surface exposed to the Martian atmosphere. Keszthelyi L. O’Connell D. R. H. Denlinger R. P. Burr D. A 2.5D Hydraulic Model for Floods in Athabasca Valles, Mars [#2245] We present initial results from the application of a new numerical model to floods in Athabasca Valles, Mars. Issues with the sparseness of MOLA data are of concern. Collier A. Sakimoto S. E. H. Grossman J. A. Silliman S. E. Parametric Study of Martian Floods at Cerberus Fossae [#2313] Recent studies of Athabasca Valles use values that may be artificially constrained. A set of Earth-derived values are proposed to be used when calculating flow rates. This will allow for the determination of the formation events of Athabasca Valles with greater accuracy. Gregoire-Mazzocco H. Stepinski T. F. McGovern P. J. Lanzoni S. Frascati A. Rinaldo A. Martian Meanders: Wavelength-Width Scaling and Flow Duration [#1185] Martian meanders reveals linear wavelength/width scaling with a coef. k~10, that can be used to estimate discharges. Simulations of channel evolution are used to determine flow duration from sinuosity. Application to Nirgal Vallis yields 200 yrs. Howard A. -
Olympus Mons
COMBAT TRANSPORT Classification: TRANSPORT Mercy Class Carries only Shields- O Class: 17 20,000mt cargo, but can carry Shield Type: EDS-5 L 5000 passengers and 1000 Model: I Shield Point Ratio: 2/1 Y Class Comission Date: 2158 medical staff. All other Stats Maximum Shield: 3 M Number Proposed: are identical Combat Efficiency 2.1 Constructed: D- 76.1 P Lost: WDF- 2.8 U Destroyed: S Scrapped: Training: M Captured: Sold: O Superstructure: 48 N Damage Chart: C S Dimensions: Length: C Width: L Height: A Discplacement: 411820 mt Cargo Specs S Total SCU: 2216 SCU S Cargo Capacity: 110800 mt Computer Type: J-5 Landing Capacity: N Cloaking Device: Power to Engage: The Olympus Mons class combat transports, Reid Fleming class deuterium tankers and Transporters- Mercy class Hospital ships marked a return to the original cargo carrying role of the Bison 6-person: design. However, unlike prewar designs these ships mounted light defensive armament. As 20-person Combat: UE Alliance forces went on the offensive in 2158, both classes helped establish a fast, 22-person Emergency: reliable logistic trail from the core areas of UE space to the front lines. cargo: Laboratories: Brigs: 37 The Olympus Mons class combat transport UES Ishtar Terra (APM-17) and the Reid Fleming Replicators: class deuterium tanker UES DeMarco (AOM-53) are now on display at the Starfleet Museum. Shuttlecraft- Commissioned Ships - Olympus Mons Class Light Shuttle: UES Olympus Mons APM-32 UES Green Mountain APM-62 Standard Shuttle: 12 UES Chomolungma APM-33 UES Qogir APM-63 Heavy Shuttle: -
Observations of Mars and Its Satellites by the Mars Imaging Camera (MIC) on Planet-B
Earth Planets Space, 50, 183–188, 1998 Observations of Mars and its satellites by the Mars Imaging Camera (MIC) on Planet-B Tadashi Mukai1, Tokuhide Akabane2, Tatsuaki Hashimoto3, Hiroshi Ishimoto1, Sho Sasaki4, Ai Inada1, Anthony Toigo5, Masato Nakamura6, Yutaka Abe6, Kei Kurita6, and Takeshi Imamura6 1The Graduate School of Science and Technology, Kobe University, Kobe 657-8501, Japan 2Hida Observatory, Kyoto University, Kamitakara, Gifu 506-13, Japan 3Institute of Space and Astronautical Science, Kanagawa 229-8510, Japan 4Geological Institute, University of Tokyo, Tokyo 113, Japan 5Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, U.S.A. 6Space and Planetary Science, University of Tokyo, Tokyo 113, Japan (Received August 7, 1997; Revised December 16, 1997; Accepted January 30, 1998) We present the specifications of the Mars Imaging Camera (MIC) on the Planet-B spin-stabilized spacecraft, and key scientific objectives of MIC observations. A non-sun-synchronous orbit of Planet-B with a large eccentricity of about 0.87 around Mars provides the opportunities (1) to observe the same region of Mars at various times of day and various solar phase angles with spatial resolution of about 60 m from a distance of 150 km altitude (at periapsis), and (2) to monitor changes of global atmospheric conditions on Mars near an apoapsis of 15 Mars radii. In addition, (3) several encounters of Planet-B with each of the two Martian satellites are scheduled during the mission lifetime of two years from October 1999 to observe their shapes and surface structures with three color filters, centered on 450, 550, and 650 nm. -
The Sand Ships of Mars By: Jeffrey D
The Sand Ships of Mars By: Jeffrey D. Beish (Rev. 12-19-2018) INTRODUCTION It was Ray Bradbury who wrote of the "Sand Ships of Mars" in his science fiction novel, The Martian Chronicles (Bradbury, 1950). One can imagine the fictional inhabitants of Mars trekking across its deserts in their floating machines stirring up huge dust devils. This great science fiction story set the stage for this author’s interest in Mars and who now writes about similar accounts of the real dusty whirlwinds on the Red Planet. [NOTE: see Mars Chart in Reference section for location names]. One of the most spectacular events to watch in our Solar System is the development of a major Martian dust storm. From Earth a Martian dust cloud may seem to be just a nuisance to any would-be telescopic explorer on that planet. However, if you consider the actual size of these clouds then you suddenly realize that many of them would cover entire western United States! Imagine if a Mars-sized planet-encircling dust storm would occur on Earth; it would blank out most of an entire Hemisphere! Some would-be Mars experts claim that after dust storms the dust settles quickly to the surface and reduces contrast of albedo features. This is contrary to the known facts; dust remains in the atmosphere of Mars for weeks -- at times months -- before settling to the surface [Pollack, 1989], [Kahn, 1992]. This dust is very fine particles of volcanic ash and when raised aloft during these storms they reach heights of several kilometers. -
The Opposition of Mars, 1999
The opposition of Mars, 1999 Richard McKim A report of the Mars Section (Director: R. J. McKim) The 1999 martian apparition was followed by BAA members while Mars Global Surveyor was monitoring the planet from martian orbit. The planet’s surface showed little change from 1997, indicating the absence of any great dust storm since solar conjunction. The long period of telescopic coverage enabled us to conclude that neither was there any planet-encircling storm in the southern martian spring or summer in 1999−2000. Three small telescopic storms were followed along the Valles Marineris, and two were seen at the edge of the summer N. polar cap. Dust storms commencing at the historically rarely-active Margaritifer Sinus emergence site (MGS data) point to ongoing changes in the fallout pattern of atmospheric dust. White cloud activity was high before and around opposition time − in northern midsummer − with morning and evening limb hazes, the equatorial cloud band (ECB) and orographic clouds. The ECB ‘season’ was identical to 1997, pointing to an equally low level of atmospheric dust-loading. Comparison with historical records suggests that the seasonal ‘wave of darkening’ may be partly attributable to the annual disappearance of the ECB. A ‘polar cyclone’ imaged by the Hubble Space Telescope between Mare Acidalium and the northern cap was followed over several days. The seasonal behaviour of the NPC, including its transition to the polar hood, was well observed. Its recession (observed from northern mid-spring) was a little slower than usual. The formation of the SPC from its winter hood, and its early recession, was also recorded. -
Present-Day Formation and Seasonal Evolution of Linear Dune Gullies on Mars Kelly Pasquon, J
Present-day formation and seasonal evolution of linear dune gullies on Mars Kelly Pasquon, J. Gargani, M. Massé, Susan J. Conway To cite this version: Kelly Pasquon, J. Gargani, M. Massé, Susan J. Conway. Present-day formation and seasonal evolution of linear dune gullies on Mars. Icarus, Elsevier, 2016, 274, pp.195-210. 10.1016/j.icarus.2016.03.024. hal-01325515 HAL Id: hal-01325515 https://hal.archives-ouvertes.fr/hal-01325515 Submitted on 8 Jan 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 Present-day formation and seasonal evolution of linear 2 dune gullies on Mars 3 Kelly Pasquona*; Julien Gargania; Marion Masséb; Susan J. Conwayb 4 a GEOPS, Univ. Paris-Sud, CNRS, University Paris-Saclay, rue du Belvédère, Bat. 5 504-509, 91405 Orsay, France 6 [email protected], [email protected] 7 8 b LPGN, University of Nantes UMR-CNRS 6112, 2 rue de la Houssinière, 44322 9 Nantes, France 10 [email protected], [email protected] 11 12 *corresponding author 1 13 Abstract 14 Linear dune gullies are a sub-type of martian gullies.