Mars Surface Change Detection from Multi-Temporal Orbital Images
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Cassis Observations of Fresh Bright Slope Streak Candidates in Arabia Terra
EPSC Abstracts Vol. 13, EPSC-DPS2019-1720-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. CaSSIS observations of fresh bright slope streak candidates in Arabia Terra A.Valantinas1, N. Thomas1, A. Pommerol1, P. Becerra1, E. Hauber2, L. L. Tornabene3, G. Cremonese4 and the CaSSIS Team1. 1Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland ([email protected]), 2Deutsches Zentrum für Luft-und Raumfahrt, Institut für Planetenforschung, Berlin, Germany, 3CPSX, Earth Sci., Western University, London, Canada, 4Osservatorio Astronomico di Padova, INAF, Padova, Italy. 1. Introduction distributions on a grid of ~16,000 hexa-gons, each 20 km in diameter. Bright slope streaks are elusive increased albedo sur- face features found on Martian slopes in low thermal 3. Results inertia regions [1, 2]. These elongated features are thought to result from the more common dark slope Our study reveals plausibly fresh bright slope streaks streaks [3, 4], which gradually fade or brighten with in several locations in Arabia Terra. For example, time [5]. Several hypotheses attempt to explain dark two images taken by CTX show a region with several slope streak origin. Dry-based models encompass dark slope streaks, but bright slope streaks in this dust mass wasting, avalanching or granular flows [1, location are only visible in CaSSIS (see Fig. 1). 6-7]. Aqueous models include subsurface aquifers, However, some bright slope streaks can be seen in lubricated dust flows and ground staining from saline both CTX frames, outside of the area shown in the fluids [8-12]. Various properties of dark slope streak figure. -
Change Detection in Mars Orbital Images Using Dynamic Landmarking
CHANGE DETECTION IN MARS ORBITAL IMAGES USING DYNAMIC LANDMARKING. Kiri L. Wagstaff1, Julian Panetta2, Adnan Ansar1, Melissa Bunte3, Ronald Greeley3, Mary Pendleton Hoffer3, and Nor- bert Schorghofer¨ 4, 1Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109 USA ([email protected]), 2California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125 USA, 3Arizona State University, School of Earth and Space Exploration, Box 871404, Tempe, AZ 85287 USA, 4University of Hawaii, Institute of Astronomy, 2680 Woodlawn Dr., Honolulu, HI 96822 USA. Introduction: As of December 2009, there are a histogram h of pixel values in a window surrounding p: more than 1,500,000 orbital images of Mars available on 255 X the Planetary Data System’s Imaging Node (from Mars S(p) = h(i)|I(p) − i|, Odyssey, Mars Express, Mars Global Surveyor, and Mars i=0 Reconnaissance Orbiter). The volume of image data is steadily increasing, as is the number of repeat images that where h(i) is the histogram count for grayscale value allow for the possibility of detecting surface changes such i and I(p) is the intensity of pixel p. Computing the as dark slope streaks [1], new impact craters and gul- salience of every pixel in the image yields a salience map. lies [2], ground ice excavated by fresh impact craters [3], To find landmarks, we specify a salience threshold to gen- etc. The number of overlapping image pairs is growing erate contours around high-salience regions. For each quickly enough that there is a need for automated meth- landmark, we extract the following attributes: mean and ods for detecting and characterizing those changes. -
The Open University | Watch?V=Sk5tpzhhw50
The Open University | watch?v=SK5tPzHHW50 [MUSIC PLAYING] KAREN FOLEY: So Jan Raack, welcome to the studio. What do you think of our audience's ideas? Aren't they creative? JAN RAACK: Of course, yes. So I joined the online chat a couple of minutes. KAREN FOLEY: I hear you've doing very well. JAN RAACK: Yeah, it was my first time-- KAREN FOLEY: Bringing some sense to the conversation, I hear. JAN RAACK: A little bit of science, yes, but not so much. Yes. KAREN FOLEY: No, that's brilliant. No, thank you. What's it like then for you? You're an academic at the Open University. You've been here not since very long. So you started here in March so it's all been quite new. What's it been like talking with-- and we've got a lot of science students out there. What's it been like as an academic then talking to everybody in this sort of environment? How have you found it? JAN RAACK: A little bit weird, to be honest, because I was a student a couple of years ago, too. And for me, it's a step further from students to ask questions-- to answer questions. So for me, it's really new and I am excited with it, really, and I enjoyed it. Yes. KAREN FOLEY: Excellent. You're now doing a lot of research. So you were from Germany and you've now come to the Open University here in sunny Milton Keynes. JAN RAACK: Sunny, yes. KAREN FOLEY: Well, not really, is it? We won't lie. -
Geomorphological Indication of Ancient, Recent, and Possibly Present-Day Aqueous Activity on Mars
地学雑誌 Journal of Geography(Chigaku Zasshi) 125(1)121–132 2016 doi:10.5026/jgeography.125.121 Geomorphological Indication of Ancient, Recent, and Possibly Present-day Aqueous Activity on Mars James M. DOHM* and Hideaki MIYAMOTO* [Received 31 March, 2015; Accepted 5 December, 2015] Abstract This paper overviews water sculpted Martian landscapes, ancient through to possibly present day, which have become more pronounced through each new orbiting, landing, and roving mission. Geomorphological evidence of ancient aqueous activity associated with lakes and putative oceans includes a diversity of features. Features include sedimentary sequences, debris flows, fluvial valleys, alluvial fans, giant polygons, and glacial and periglacial landscapes. Arguably one of the most significant geomorphological indicators of a paleoocean is deltaic landforms identified along a topographic zonal boundary which correlates with reported putative shorelines. Other evidence includes distinct geochemical/mineralogical/elemental signatures of aqueous weathering. In addition, relatively high-resolution imaging cameras onboard the Mars Global Surveyor, Mars Odyssey, and Mars Reconnaissance Orbiter have detailed features which indicate recent and possibly present-day aqueous activity such as slope streaks, slope linea, gullies which occur along faults and fractures and source from geologic contacts and tectonic structures, and possible open-system pingos, among other feature types. Ancient, recent, and possibly present-day features point to both surface and subsurface aqueous environments throughout time, and thus making Mars a prime target to address the ever- important question of whether life exists beyond the Earth. Key words: Mars, geomorphology, hydrology, oceans, outflow channel, gullies, slope linea Mitchell and Wilson, 2003). Perhaps the most I.Introduction surprising finding from the post-Viking mission Mars' missions continue to reveal aqueous- are a variety of features that indicate the Mars modified Martian landscapes. -
Field Measurements of Terrestrial and Martian Dust Devils Journal Item
Open Research Online The Open University’s repository of research publications and other research outputs Field Measurements of Terrestrial and Martian Dust Devils Journal Item How to cite: Murphy, Jim; Steakley, Kathryn; Balme, Matt; Deprez, Gregoire; Esposito, Francesca; Kahanpää, Henrik; Lemmon, Mark; Lorenz, Ralph; Murdoch, Naomi; Neakrase, Lynn; Patel, Manish and Whelley, Patrick (2016). Field Measurements of Terrestrial and Martian Dust Devils. Space Science Reviews, 203(1) pp. 39–87. For guidance on citations see FAQs. c 2016 Springer https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Accepted Manuscript Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1007/s11214-016-0283-y Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk 1 Field Measurements of Terrestrial and Martian Dust Devils 2 Jim Murphy1, Kathryn Steakley1, Matt Balme2, Gregoire Deprez3, Francesca 3 Esposito4, Henrik Kahapää5, Mark Lemmon6, Ralph Lorenz7, Naomi Murdoch8, Lynn 4 Neakrase1, Manish Patel2, Patrick Whelley9 5 1-New Mexico State University, Las Cruces NM, USA 2 - Open University, Milton Keynes UK 6 3 - Laboratoire Atmosphères, Guyancourt, France 4 - INAF - Osservatorio Astronomico di 7 Capodimonte, Naples, Italy 5 - Finnish Meteorological Institute, Helsinki, Finland 6 - Texas 8 A&M University, College Station TX, USA 7 -Johns Hopkins University Applied Physics Lab, 9 Laurel MD USA 8 - ISAE-SUPAERO, Toulouse University, France 9 - NASA Goddard 10 Space Flight Center, Greenbelt MD, USA 11 submitted to SSR 10 May, 2016 12 Revised manuscript 08 August 2016 13 ABSTRACT 14 Surface-based measurements of terrestrial and martian dust devils/convective vortices 15 provided from mobile and stationary platforms are discussed. -
DRY (?) MARS: AEOLIAN PROCESSES, MASS WASTING, and ROCKS 7:00 P.M
Lunar and Planetary Science XXXVI (2005) sess44.pdf Tuesday, March 15, 2005 POSTER SESSION I: DRY (?) MARS: AEOLIAN PROCESSES, MASS WASTING, AND ROCKS 7:00 p.m. Fitness Center Mullins K. F. Hayward R. K. Titus T. N. Bourke M. C. Fenton L. K. Mars Digital Dune Database: A Quantitative Look at the Geographic Distribution of Dunes on Mars [#1986] Initial steps in developing a digital dune database in a global geographic context for Mars have been completed. This database currently contains information delineating the dune fields between ±65 degrees latitude. Banks M. Bridges N. T. Benzit M. Measurements of the Coefficient of Restitution of Quartz Sand on Basalt: Implications for Abrasion Rates on Earth and Mars [#2116] Using high speed video to assess grain-rock interactions, it was found that the KE lost on impact is generally proportional to incoming velocity and impact angle, but that only a fraction of this energy goes into direct abrasion of the rock surface. Neakrase L. D. V. Greeley R. Williams D. A. Reiss D. Michaels T. I. Rafkin S. C. R. Neukum G. HRSC Team Hecates Tholus, Mars: Nighttime Aeolian Activity Suggested by Thermal Images and Mesoscale Atmospheric Model Simulations [#1898] Previously unidentified wind streaks identified on nighttime IR images on Hecates Tholus volcano on Mars agree with predictions of nighttime patterns by an atmospheric model, suggesting that nighttime winds are responsible for modifying the surface in contrast to afternoon winds. Neakrase L. D. V. Greeley R. Iversen J. D. Balme M. R. Foley D. J. Eddlemon E. E. Dust Devils on Mars: Effects of Surface Roughness on Particle Threshold [#1857] The aim of this study is to determine experimentally the effects of non-erodable roughness elements on vortex particle threshold through laboratory simulations of natural surfaces pertaining to dust devils on Earth and Mars. -
Detecção Automática E Análise Temporal De Slope Streaks Na Superfície De Marte
UNIVERSIDADE ESTADUAL PAULISTA Faculdade de Ciências e Tecnologia Programa de Pós-Graduação em Ciências Cartográficas FERNANDA PUGA SANTOS CARVALHO DETECÇÃO AUTOMÁTICA E ANÁLISE TEMPORAL DE SLOPE STREAKS NA SUPERFÍCIE DE MARTE TESE Presidente Prudente 2016 FERNANDA PUGA SANTOS CARVALHO DETECÇÃO AUTOMÁTICA E ANÁLISE TEMPORAL DE SLOPE STREAKS NA SUPERFÍCIE DE MARTE Tese apresentada ao Programa de Pós-Graduação em Ciências Cartográficas para a obtenção do título de doutor pela Faculdade de Ciências e Tecnologia da Universidade Estadual Paulista “Júlio de Mesquita Filho” Campus de Presidente Prudente. Área de concentração: Computação de Imagens Orientador: Professor Titular Erivaldo Antônio da Silva. Coorientador: Dr. Pedro Miguel Berardo Duarte Pina. Presidente Prudente Março de 2016 FICHA CATALOGRÁFICA Carvalho, Fernanda Puga Santos. C323d Detecção automática e análise temporal de slope streaks na superfície de Marte / Fernanda Puga Santos Carvalho. - Presidente Prudente : [s.n], 2016 76 f. : il. Orientador: Erivaldo Antônio da Silva Coorientador: Pedro Miguel Berardo Duarte Pina Tese (doutorado) - Universidade Estadual Paulista, Faculdade de Ciências e Tecnologia Inclui bibliografia 1. Slope streaks. 2. Detecção automática. 3. Análise temporal. I. Carvalho, Fernanda Puga Santos. II. Silva, Erivaldo Antônio da III. Pina, Pedro Miguel Berardo Duarte. IV. Universidade Estadual Paulista. Faculdade de Ciências e Tecnologia. V. Detecção automática e análise temporal de slope streaks na superfície de Marte. AGRADECIMENTOS Gostaria de registrar o meu sincero agradecimento a todos que contribuíram de forma direta e indireta para o desenvolvimento deste trabalho. À minha família, em especial ao meu marido André, cujo apoio e incentivo incondicional foram fundamentais para realização deste meu sonho. Ao professor Erivaldo, pela confiança na minha capacidade em desenvolver uma tese de doutorado e pelo apoio de sempre. -
Modeling the Development of Martian Sublimation Thermokarst Landforms
Icarus 262 (2015) 154–169 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Modeling the development of martian sublimation thermokarst landforms a, b b Colin M. Dundas ⇑, Shane Byrne , Alfred S. McEwen a Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA article info abstract Article history: Sublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsur- Received 8 August 2014 face. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the mid- Revised 17 June 2015 latitudes and considered likely thermokarst features. We describe a landscape evolution model that cou- Accepted 29 July 2015 ples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens of thou- Available online 21 August 2015 sands of Mars years under conditions similar to the present, the model produces scallop-like features similar to those on the martian surface, starting from much smaller initial disturbances. The model also Keywords: indicates crater expansion when impacts occur in surfaces underlain by excess ice to some depth, with Mars, surface morphologies similar to observed landforms on the martian northern plains. In order to produce these Geological processes Mars, climate landforms by sublimation, substantial quantities of excess ice are required, at least comparable to the vertical extent of the landform, and such ice must remain in adjacent terrain to support the non- deflated surface. We suggest that martian thermokarst features are consistent with formation by subli- mation, without melting, and that significant thicknesses of very clean excess ice (up to many tens of meters, the depth of some scalloped depressions) are locally present in the martian mid-latitudes. -
Download the Acquired Data Or to Fix Possible Problem
Università degli Studi di Napoli Federico II DOTTORATO DI RICERCA IN FISICA Ciclo 30° Coordinatore: Prof. Salvatore Capozziello Settore Scientifico Disciplinare FIS/05 Characterisation of dust events on Earth and Mars the ExoMars/DREAMS experiment and the field campaigns in the Sahara desert Dottorando Tutore Gabriele Franzese dr. Francesca Esposito Anni 2014/2018 A birbetta e giggione che sono andati troppo veloci e a patata che invece adesso va piano piano Summary Introduction ......................................................................................................................... 6 Chapter 1 Atmospheric dust on Earth and Mars............................................................ 9 1.1 Mineral Dust ....................................................................................................... 9 1.1.1 Impact on the Terrestrial land-atmosphere-ocean system .......................... 10 1.1.1.1 Direct effect ......................................................................................... 10 1.1.1.2 Semi-direct and indirect effects on the cloud physics ......................... 10 1.1.1.3 Indirect effects on the biogeochemical system .................................... 11 1.1.1.4 Estimation of the total effect ............................................................... 11 1.2 Mars .................................................................................................................. 12 1.2.1 Impact on the Martian land-atmosphere system ......................................... 13 1.3 -
Dust Devil Track Survey at the Insight Landing Sites: Implications for the Probability of Solar Panel Clearing Events
46th Lunar and Planetary Science Conference (2015) 2070.pdf DUST DEVIL TRACK SURVEY AT THE INSIGHT LANDING SITES: IMPLICATIONS FOR THE PROBABILITY OF SOLAR PANEL CLEARING EVENTS. D. Reiss1 and R. D. Lorenz2, Institut für Planeto- logie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany, 2Johns Hopkins Uni- versity Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA. Introduction: The InSight robotic lander is scheduled Morphology. Fig. 2 shows an example of a typical newly to land on Mars in September 2016. InSight was designed to formed DDT. The DDTs in the study region are relatively perform the first comprehensive surface-based geophysical straight which is also expressed in their low mean sinuosity investigation of Mars [1]. Passage of vortices may have a of 1.03 (standard deviation = 0.004). The sinuosity is lower number of influences on the geophysical measurements to be compared to mean values of ~1.3 and ~1.08 measured by [8] made by InSight. Seismic data could be influenced by dust in Russell and Gusev crater, respectively. devils and vortices via several mechanisms such as loading of the elastic ground by a surface pressure field which causes a local tilt [e.g. 2]. In addition, the power supply of the In- Sight instruments is provided by solar arrays. Solar-powered missions on Mars like the Sojourner rover in 1997 were af- fected by a decline in electrical power output by 0.2-0.3 % per day caused by steadily dust deposition on its horizontal Fig. 2. Example of observed track formation between HiRISE imag- solar panel [3]. -
Scalloped Terrains in the Peneus and Amphitrites Paterae Region of Mars As Observed by Hirise
Icarus 205 (2010) 259–268 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE A. Lefort *, P.S. Russell, N. Thomas Space Research and Planetary Sciences, Physikalisches Institut, Universität Bern, 3012 Bern, Switzerland article info abstract Article history: The Peneus and Amphitrites Paterae region of Mars displays large areas of smooth, geologically young Received 10 October 2008 terrains overlying a rougher and older topography. These terrains may be remnants of the mid-latitude Revised 15 May 2009 mantle deposit, which is thought to be composed of ice-rich material originating from airfall deposition Accepted 3 June 2009 during a high-obliquity period less than 5 Ma ago. Within these terrains, there are several types of poten- Available online 14 June 2009 tially periglacial features. In particular, there are networks of polygonal cracks and scalloped-shaped depressions, which are similar to features found in Utopia Planitia in the northern hemisphere. This area Keywords: also displays knobby terrain similar to the so-called ‘‘basketball terrains” of the mid and high martian lat- Mars, Surface itudes. We use recent high resolution images from the High Resolution Imaging Science Experiment (HiR- Geological processes Ices ISE) along with data from previous Mars missions to study the small-scale morphology of the scalloped terrains, and associated polygon network and knobby terrains. We compare these with the features observed in Utopia Planitia and attempt to determine their formation process. While the two sites share many general features, scallops in Peneus/Amphitrites Paterae lack the diverse polygon network (i.e. -
Automatic Detection of Martian Dark Slope Streaks by Machine Learning Using Hirise Images ⇑ Yexin Wang, Kaichang Di , Xin Xin, Wenhui Wan
ISPRS Journal of Photogrammetry and Remote Sensing 129 (2017) 12–20 Contents lists available at ScienceDirect ISPRS Journal of Photogrammetry and Remote Sensing journal homepage: www.elsevier.com/locate/isprsjprs Automatic detection of Martian dark slope streaks by machine learning using HiRISE images ⇑ Yexin Wang, Kaichang Di , Xin Xin, Wenhui Wan State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, No. 20A, Datun Road, Chaoyang District, Beijing 100101, China article info abstract Article history: Dark slope streaks (DSSs) on the Martian surface are one of the active geologic features that can be Received 13 January 2016 observed on Mars nowadays. The detection of DSS is a prerequisite for studying its appearance, morphol- Received in revised form 15 March 2017 ogy, and distribution to reveal its underlying geological mechanisms. In addition, increasingly massive Accepted 24 April 2017 amounts of Mars high resolution data are now available. Hence, an automatic detection method for locat- ing DSSs is highly desirable. In this research, we present an automatic DSS detection method by combin- ing interest region extraction and machine learning techniques. The interest region extraction combines Keywords: gradient and regional grayscale information. Moreover, a novel recognition strategy is proposed that Dark slope streak takes the normalized minimum bounding rectangles (MBRs) of the extracted regions to calculate the Martian surface Machine learning Local Binary Pattern (LBP) feature and train a DSS classifier using the Adaboost machine learning algo- HiRISE image rithm. Comparative experiments using five different feature descriptors and three different machine Region detection learning algorithms show the superiority of the proposed method.