High-Resolution Thermal-Inertia Mapping of Mars: Sites of Exobiological Interest
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Watershed Modeling in the Tyrrhena Terra Region of Mars Scott C
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09001, doi:10.1029/2009JE003429, 2010 Watershed modeling in the Tyrrhena Terra region of Mars Scott C. Mest,1,2 David A. Crown,1 and William Harbert3 Received 9 May 2009; revised 13 December 2009; accepted 29 January 2010; published 1 September 2010. [1] Watershed analyses from high‐resolution image (Viking, Mars Orbiter Camera, and Thermal Emission Imaging System) and topographic (Mars Orbiter Laser Altimeter [MOLA]) data are used to qualitatively and quantitatively characterize highland fluvial systems and analyze the role of water in the evolution of Tyrrhena Terra (13°S–30°S, 265°W–280°W), Mars. In this study, Geographical Information System software is used in conjunction with MOLA Digital Elevation Models to delineate drainage basin divides, extract valley networks, and derive basin and network morphometric parameters (e.g., drainage density, stream order, bifurcation ratio, and relief morphometry) useful in characterizing the geologic and climatic conditions of watershed formation, as well as for evaluating basin “maturity” and processes of watershed development. Model‐predicted valley networks and watershed boundaries, which are dependent on the degree to which pixel sinks are filled in the topographic data set and a channelization threshold, are evaluated against image and topographic data, slope maps, and detailed maps of valley segments from photogeologic analyses. Valley morphologies, crater/valley relationships, and impact crater distributions show that valleys in Tyrrhena Terra are ancient. Based on geologic properties of the incised materials, valley and network morphologies, morphometric parameters, and the presence of many gullies heading at or near‐crater rim crests, surface runoff, derived from rainfall or snowmelt, was the dominant erosional process; sapping may have only played a secondary role in valley formation in Tyrrhena Terra. -
Diverse Morphology and Mineralogy of Aqueous Outcrops at Libya Montes, Mars D
46th Lunar and Planetary Science Conference (2015) 1738.pdf DIVERSE MORPHOLOGY AND MINERALOGY OF AQUEOUS OUTCROPS AT LIBYA MONTES, MARS D. Tirsch1, J. L. Bishop1,2, J. Voigt1,3, L. L. Tornabene4, G. Erkeling5, H. Hiesinger5 and R. Jaumann1,3 1Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany, [email protected]. 2Carl Sagan Center, SETI Institute, Mountain View, CA, USA.3Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany. 4Dept. of Earth Sciences, Centre for Planetary Science and Exploration, University of Western Ontario, London, Canada. 5Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Germany. Introduction: The Libya Montes are part of about the geological history of the study site in context the southern rim-complex of the Isidis impact basin on with regionally acting modification processes. Mars. The region is characterized by pre-Noachian and Methods: We performed a photogeological Noachian aged highland rocks alternating with multiple mapping, as well as morphological and spectral sedimentary units of Noachian to Amazonian age, analyses on a variety of datasets. HRSC topography some of them heavily dissected by dense valley (50 m/px), HiRISE and CTX imagery (25 cm/px and networks [1 - 7]. The region experienced a complex 6 m/px), and CRISM spectral data (18/33.8 m/px) have history of impact, volcanic, tectonic, fluvial and been used to reveal the geological setting of the region. aeolian modification processes resulting in the geology Specific geologic units indicated by CRISM mineral observed today. Ancient aqueous outcrops have been maps derived from spectral parameter products (R: identified by coordinated spectral and geological BD2300, G: OLV, B: LCP), have been evaluated analyses at various locations in the region [7]. -
Geologic Context of Lacustrine Mineral Deposits at Bradbury Crater, Mars
47th Lunar and Planetary Science Conference (2016) 1444.pdf GEOLOGIC CONTEXT OF LACUSTRINE MINERAL DEPOSITS AT BRADBURY CRATER, MARS. D. Tirsch1, G. Erkeling2, J. L. Bishop3, L. L. Tornabene4, H. Hiesinger2 and R. Jaumann1,5 1Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany ([email protected]). 2Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Germany. 3Carl Sagan Center, SETI Institute, Mountain View, CA, USA. 4Dept. of Earth Sciences, Centre for Planetary Science and Exploration, University of Western Ontario, London, Canada. 5Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany. Introduction: The 60-km Bradbury Crater Methods: Geological analyses have been (85.8°E; 2.7°N) is located at the Libya Montes region performed on the basis of CTX and HiRISE image data at the southern rim of the Isidis impact basin on Mars. in combination with HRSC and HiRISE digital This area is predominantly characterized by Noachian- elevation models. Mineral detection has been aged highland massifs that were heavily modified by performed by spectral analyses of targeted CRISM fluvial, lacustrine, aeolian, volcanic, and impact images. Spectral images are processed for instrumental processes occurring in multiple recurring events [e.g., effects, converted to I/F and atmospheric components 1-7]. Bradbury Crater stands out for its abundance of are minimized using a ratio with a CRISM scene of fluvial and lacustrine landforms, which reflect a varied Olympus Mons [9]. Ratios to spectrally neutral regions history of aqueous-related geological processes [5,8]. in the same column are employed to emphasize A 2.8 by 5 km-sized fan-shaped deposit has been spectral absorption features due to distinctive minerals. -
Endogenic and Exogenic Contributions to Visible-Wavelength Spectra of Europa’S Trailing Hemisphere
Preprint typeset using LATEX style AASTeX6 v. 1.0 ENDOGENIC AND EXOGENIC CONTRIBUTIONS TO VISIBLE-WAVELENGTH SPECTRA OF EUROPA'S TRAILING HEMISPHERE Samantha K. Trumbo, Michael E. Brown Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA Kevin P. Hand Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA ABSTRACT The composition of Europa's trailing hemisphere reflects the combined influences of endogenous geo- logic resurfacing and exogenous sulfur radiolysis. Using spatially resolved visible-wavelength spectra of Europa obtained with the Hubble Space Telescope, we map multiple spectral features across the trailing hemisphere and compare their geographies with the distributions of large-scale geology, mag- netospheric bombardment, and surface color. Based on such comparisons, we interpret some aspects of our spectra as indicative of purely exogenous sulfur radiolysis products and other aspects as in- dicative of radiolysis products formed from a mixture of endogenous material and magnetospheric sulfur. The spatial distributions of two of the absorptions seen in our spectra|a widespread down- turn toward the near-UV and a distinct feature at 530 nm|appear consistent with sulfur allotropes previously suggested from ground-based spectrophotometry. However, the geographies of two addi- tional features|an absorption feature at 360 nm and the spectral slope at red wavelengths|are more consistent with endogenous material that has been altered by sulfur radiolysis. We suggest irradiated sulfate salts as potential candidates for this material, but we are unable to identify particular species with the available data. Keywords: planets and satellites: composition | planets and satellites: individual (Europa) | planets and satellites: surfaces 1. -
Valleys in the Martian Libya Montes: Evidence for Episodic Erosion Events R
41st Lunar and Planetary Science Conference (2010) 1629.pdf Valleys in the Martian Libya Montes: Evidence for episodic erosion events R. Jaumann1,2, A. Nass1,3, D. Tirsch1, D. Reiss4, and G. Neukum2 1DLR, Inst. of Planet. Expl. Rutherfordstrasse 2, 12489 Berlin, Germany; 2Dept. of Earth Sciences, Inst. of Geosciences, Remote Sensing of the Earth and Planets, Freie Universitaet Berlin, Germany; 3Dept. of Geography, Geomatics Section, Universität Potsdam, Germany; 4Inst. of Planetology, Westfälische Wilhelms-Universität, Münster, Germany; ([email protected]). Introduction: Martian valley networks have been (Fig.1) originates at 80° E, 0.7° S in a region that is cited as the best evidence that Mars maintained flow of affected by Syrtis Major lava flows. liquid water across its surface. Although internal structures associated with a fluvial origin within valleys such as inner channels, terraces, slip-off and undercut slopes are extremely rare on Mars (Carr and Malin, 2000) such features can be identified in high- resolution imagery (e.g. Malin and Edgett, 2001; Jaumann et al., 2005). However, besides internal features the source regions are an important indicator for the flow processes in Martian valleys because they define the drainage area and thus constrain the amount of available water for eroding the valley network. The three-dimensional highly resolved data of the High Resolution Stereo Camera (HRSC) on the Mars Express Mission (Jaumann et al., 2007) allow the detailed examination of valley network source regions. Western Libya Montes: The Libya Montes (Fig. 1), at about 79° E to 84° E and 1.5° S to 4.5° N, border the southern margin of the Isidis Planitia rim. -
Journal of Geophysical Research
Journal Code Article ID Dispatch: 05.12.18 CE: MAS Revised proofs are sent only in the case of J G R E 21053No.ofPages: 21 ME: extensive corrections upon request 1 2 3 4 5 Journal of Geophysical Research: Planets 6 7 RESEARCH ARTICLE Evolution of Escarpments, Pediments, and Plains 8 9 10.1029/2018JE005681 in the Noachian Highlands of Mars 10 11 1 1 Key Points: Jon C. Cawley and Rossman P. Irwin III Q212 Q3 • Debris-mantled escarpments, Q5 13 regolith pediments, sloping 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA aggradational surfaces, and 14 depositional plains formed on 15 Martian cratered terrain 16 • Noachian arid-zone geomorphology Abstract Extensive Noachian-aged intercrater planation surfaces comprise much of the southern included aqueous weathering of highlands of Mars. We mapped aggradational and stable to degradational surfaces in three study areas 17 basalt to fines, low-intensity fluvial with diverse relief elements and ages: the high and rugged relief of Libya Montes, the well-preserved 18 erosion, and deposition in basins 19 intercrater plains of Noachis Terra, and the rolling relief with more drainage development in Terra Cimmeria. • These processes smoothed and 20 sealed Noachian ejecta blankets, Here we describe four major geomorphic features that formed in these regions: debris-mantled escarpments, 21 which required little geomorphic regolith pediments, sloping aggradational surfaces, and depositional plains. We interpret that with tectonic work to form stable pediments 22 stability and an arid paleoclimate, these features supported slow pedogenesis, sediment transport, and 23 diagenesis over hundreds of millions of years during heavy impact bombardment. -
Schmidt Et Al
Earth and Planetary Science Letters 384 (2013) 37–41 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Detectability of thermal signatures associated with active formation of ‘chaos terrain’ on Europa ∗ Oleg Abramov a, , Julie A. Rathbun b, Britney E. Schmidt c,JohnR.Spencerd a U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA b Planetary Science Institute, 1700 E. Fort Lowell Rd., Suite 106, Tucson, AZ 85719-2395, USA c Georgia Institute of Technology, School of Earth and Atmospheric Sciences, 311 Ferst Dr., Atlanta, GA 30312, USA d Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, USA article info abstract Article history: A recent study by Schmidt et al. (2011) suggests that Thera Macula, one of the “chaos regions” on Europa, Received 21 February 2013 may be actively forming over a large liquid water lens. Such a process could conceivably produce a Received in revised form 12 September thermal anomaly detectable by a future Europa orbiter or flyby mission, allowing for a direct verification 2013 of this finding. Here, we present a set of models that quantitatively assess the surface and subsurface Accepted 20 September 2013 temperatures associated with an actively resurfacing chaos region using constraints from Thera Macula. Available online 26 October 2013 Editor: C. Sotin The results of this numerical study suggest that the surface temperature over an active chaos region can be as high as ∼200 K. However, low-resolution Galileo Photo-Polarimeter Radiometer (PPR) observations Keywords: indicate temperatures below 120 K over Thera Macula. -
Libya Montes and Northwestern Tyrrhena Terra
The 1:1,000,000-Scale Geology of Western Libya Montes and Northwestern Tyrrhena Terra Alexandra Huff and James Skinner, Jr. Astrogeology Science Center U. S. Geological Survey Planetary Geologic Mappers Meeting 2017 Quadrangle Location • 6 MTM quads covering the highland lowland transition from Tyrrhena Terra to Isidis Planitia • Improved understanding of this area will provide insight into the evolution of ancient Martian highlands Previous Mapping • USGS maps • 1:20M Global Map (Tanaka et al., 2014) • 1:15M Eastern Region of Mars (Greeley and Guest, 1987) • 1:5M Syrtis Major Quadrangle (Meyer and Grolier, 1977) • 1:5M Iapygia Quadrangle (Schaber, 1977) • Topic-based Maps • Crumpler and Tanaka, 2003 (blue) • Jaumann et al., 2010 (red) • Bishop et al., 2013 (purple) Regional geology questions: How many massif units are there? How many channelization periods were there? What is the history of the intermediate cratered plains? PGM2017 Abstract #7112 Our Map Purpose: We are filling this scale-based gap in understanding by assembling a 1:1M scale geologic map to bridge existing global and local schemata. • Methodology • 1:250,000 mapping scale • THEMIS Daytime IR base map • Supplemented with MOLA, CTX, and THEMIS Nighttime IR data sets Unit Mapping: Grouping • 4 Unit Groups • Impact crater units (blue) • Older massif group (brown) • Intermediate-aged terra group (tan) • Younger plains group (green) Unit Mapping: Impact Crater Units Crater Unit 1/ Crater Units Smooth Crater Infill Crater Unit 2 Crater Unit 3 Differentiated c2 c3 c1 cs Unit -
Liquid Water on Mars
Report, Planetary Sciences Unit (AST80015), Swinburne Astronomy Online Preprint typeset using LATEX style emulateapj v. 12/16/11 LIQUID WATER ON MARS M. Usatov1 Report, Planetary Sciences Unit (AST80015), Swinburne Astronomy Online ABSTRACT Geomorphological, mineralogical and other evidence of the conditions favoring the existence of water on Mars in liquid phase is reviewed. This includes signatures of past and, possibly, present aqueous environments, such as the northern ocean, lacustrine environments, sedimentary and thermokarst landforms, glacial activity and water erosion features. Reviewed also are hydrous weathering processes, observed on surface remotely and also via analysis of Martian meteorites. Chemistry of Martian water is discussed: the triple point, salts and brines, as well as undercooled liquid interfacial and solid-state greenhouse effect melted waters that may still be present on Mars. Current understanding of the evolution of Martian hydrosphere over geological timescales is presented from early period to the present time, along with the discussion of alternative interpretations and possibilities of dry and wet Mars extremes. 1. INTRODUCTION morphological and mineralogical evidence of aqueous en- The presence of water on Earth, as seen from space, vironments available in the past and, possibly, present can be implied from the observations of low-albedo fea- time is presented in x3 which will be correlated with the tures, like seas and oceans, fluvial features on its sur- current understanding of the evolution of Martian hy- face, atmospheric phenomena, polar ice caps, and the drosphere at x4. Alternative (dry) interpretations of the snow cover exhibiting seasonal variations, not to mention evidence are discussed in x5. spectroscopy. -
Rapid Single Image-Based DTM Estimation from Exomars TGO Cassis Images Using Generative Adversarial U-Nets
remote sensing Article Rapid Single Image-Based DTM Estimation from ExoMars TGO CaSSIS Images Using Generative Adversarial U-Nets Yu Tao 1,* , Siting Xiong 2, Susan J. Conway 3, Jan-Peter Muller 1 , Anthony Guimpier 3, Peter Fawdon 4, Nicolas Thomas 5 and Gabriele Cremonese 6 1 Mullard Space Science Laboratory, Imaging Group, Department of Space and Climate Physics, University College London, Holmbury St Mary, Surrey RH5 6NT, UK; [email protected] 2 College of Civil and Transportation Engineering, Shenzhen University, Shenzhen 518060, China; [email protected] 3 Laboratoire de Planétologie et Géodynamique, CNRS, UMR 6112, Universités de Nantes, 44300 Nantes, France; [email protected] (S.J.C.); [email protected] (A.G.) 4 School of Physical Sciences, Open University, Walton Hall, Milton Keynes MK7 6AA, UK; [email protected] 5 Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland; [email protected] 6 INAF, Osservatorio Astronomico di Padova, 35122 Padova, Italy; [email protected] * Correspondence: [email protected] Abstract: The lack of adequate stereo coverage and where available, lengthy processing time, various artefacts, and unsatisfactory quality and complexity of automating the selection of the best set of processing parameters, have long been big barriers for large-area planetary 3D mapping. In this paper, Citation: Tao, Y.; Xiong, S.; Conway, we propose a deep learning-based solution, called MADNet (Multi-scale generative Adversarial S.J.; Muller, J.-P.; Guimpier, A.; u-net with Dense convolutional and up-projection blocks), that avoids or resolves all of the above Fawdon, P.; Thomas, N.; Cremonese, G. -
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. -
Morphologic, Stratigraphic and Morphometric Investigations in Eastern Libya Montes, Mars: Implications for Long-Term Fluvial Activity
40th Lunar and Planetary Science Conference (2009) 1604.pdf MORPHOLOGIC, STRATIGRAPHIC AND MORPHOMETRIC INVESTIGATIONS IN EASTERN LIBYA MONTES, MARS: IMPLICATIONS FOR LONG-TERM FLUVIAL ACTIVITY. G. Erkeling 1, D. Reiss 1, H. Hiesinger 1, R. Jaumann 2,3 1Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Ger- many, 2Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany. 3Department of Earth Sciences, Institute of Geological Sciences, Planetary Sciences and Remote Sensing, Free University Berlin, Berlin, Germany. ([email protected]/ Fax: +49-251-8336376) Introduction: The Noachian highlands of Libya measured in the “Noachian massifs” (Nm) with a range Montes, located at the southern edge of Isidis Planitia, from ~4.1 to ~3.8 Ga and an average age of ~4.0 Ga. represent one of the oldest regions on Mars [1] that The “dendritic valley networks” show the same average have been degraded by intensive, long-term and repeated age of ~4.0 Ga, which corresponds to a formation fluvial processes which led to the formation of “dendritic within the middle Noachian. Our crater counts reveal valley networks” [2-5]. Widespread “dendritic valley that the formation of the dendritic drainage patterns networks”, particularly their extended branching were occurred within ~300 My, between ~4.1 and ~3.8 Ga. interpreted as evidence for atmospheric precipitation [2-5]. Within the Libya Montes, three distinct valley systems are defined by [2]: a western, a central and an eastern system. Here, we present our morphologic and strati- graphic investigations of the eastern valley system lo- cated between 87˚E and 90˚E and 5˚S and 5˚N.