Theoretical Comparisons of the Concentration-Dependent Diffusion
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SPACE RESEARCH in POLAND Report to COMMITTEE
SPACE RESEARCH IN POLAND Report to COMMITTEE ON SPACE RESEARCH (COSPAR) 2020 Space Research Centre Polish Academy of Sciences and The Committee on Space and Satellite Research PAS Report to COMMITTEE ON SPACE RESEARCH (COSPAR) ISBN 978-83-89439-04-8 First edition © Copyright by Space Research Centre Polish Academy of Sciences and The Committee on Space and Satellite Research PAS Warsaw, 2020 Editor: Iwona Stanisławska, Aneta Popowska Report to COSPAR 2020 1 SATELLITE GEODESY Space Research in Poland 3 1. SATELLITE GEODESY Compiled by Mariusz Figurski, Grzegorz Nykiel, Paweł Wielgosz, and Anna Krypiak-Gregorczyk Introduction This part of the Polish National Report concerns research on Satellite Geodesy performed in Poland from 2018 to 2020. The activity of the Polish institutions in the field of satellite geodesy and navigation are focused on the several main fields: • global and regional GPS and SLR measurements in the frame of International GNSS Service (IGS), International Laser Ranging Service (ILRS), International Earth Rotation and Reference Systems Service (IERS), European Reference Frame Permanent Network (EPN), • Polish geodetic permanent network – ASG-EUPOS, • modeling of ionosphere and troposphere, • practical utilization of satellite methods in local geodetic applications, • geodynamic study, • metrological control of Global Navigation Satellite System (GNSS) equipment, • use of gravimetric satellite missions, • application of GNSS in overland, maritime and air navigation, • multi-GNSS application in geodetic studies. Report -
Mawrth Vallis, Mars: a Fascinating Place for Future in Situ Exploration
Mawrth Vallis, Mars: a fascinating place for future in situ exploration François Poulet1, Christoph Gross2, Briony Horgan3, Damien Loizeau1, Janice L. Bishop4, John Carter1, Csilla Orgel2 1Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France 2Institute of Geological Sciences, Planetary Sciences and Remote Sensing Group, Freie Universität Berlin, Germany 3Purdue University, West Lafayette, USA. 4SETI Institute/NASA-ARC, Mountain View, CA, USA Corresponding author: François Poulet, IAS, Bâtiment 121, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France; email: [email protected] Running title: Mawrth: a fascinating place for exploration 1 Abstract After the successful landing of the Mars Science Laboratory rover, both NASA and ESA initiated a selection process for potential landing sites for the Mars2020 and ExoMars missions, respectively. Two ellipses located in the Mawrth Vallis region were proposed and evaluated during a series of meetings (3 for Mars2020 mission and 5 for ExoMars). We describe here the regional context of the two proposed ellipses as well as the framework of the objectives of these two missions. Key science targets of the ellipses and their astrobiological interests are reported. This work confirms the proposed ellipses contain multiple past Martian wet environments of subaerial, subsurface and/or subaqueous character, in which to probe the past climate of Mars, build a broad picture of possible past habitable environments, evaluate their exobiological potentials and search for biosignatures in well-preserved rocks. A mission scenario covering several key investigations during the nominal mission of each rover is also presented, as well as descriptions of how the site fulfills the science requirements and expectations of in situ martian exploration. -
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. -
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, -
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. -
Bio-Preservation Potential of Sediment in Eberswalde Crater, Mars
Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Fall 2020 Bio-preservation Potential of Sediment in Eberswalde crater, Mars Cory Hughes Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Hughes, Cory, "Bio-preservation Potential of Sediment in Eberswalde crater, Mars" (2020). WWU Graduate School Collection. 992. https://cedar.wwu.edu/wwuet/992 This Masters Thesis is brought to you for free and open access by the WWU Graduate and Undergraduate Scholarship at Western CEDAR. It has been accepted for inclusion in WWU Graduate School Collection by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. Bio-preservation Potential of Sediment in Eberswalde crater, Mars By Cory M. Hughes Accepted in Partial Completion of the Requirements for the Degree Master of Science ADVISORY COMMITTEE Dr. Melissa Rice, Chair Dr. Charles Barnhart Dr. Brady Foreman Dr. Allison Pfeiffer GRADUATE SCHOOL David L. Patrick, Dean Master’s Thesis In presenting this thesis in partial fulfillment of the requirements for a master’s degree at Western Washington University, I grant to Western Washington University the non-exclusive royalty-free right to archive, reproduce, distribute, and display the thesis in any and all forms, including electronic format, via any digital library mechanisms maintained by WWU. I represent and warrant this is my original work, and does not infringe or violate any rights of others. I warrant that I have obtained written permissions from the owner of any third party copyrighted material included in these files. -
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. -
Possible Evaporite Karst in an Interior Layered Deposit in Juventae
International Journal of Speleology 46 (2) 181-189 Tampa, FL (USA) May 2017 Available online at scholarcommons.usf.edu/ijs International Journal of Speleology Off icial Journal of Union Internationale de Spéléologie Possible evaporite karst in an interior layered deposit in Juventae Chasma, Mars Davide Baioni* and Mario Tramontana Planetary Geology Research Group, Dipartimento di Scienze Pure e Applicate (DiSPeA), Università degli Studi di Urbino "Carlo Bo", Campus Scientifico Enrico Mattei, 61029 Urbino (PU), Italy Abstract: This paper describes karst landforms observed in an interior layered deposit (ILD) located within Juventae Chasma a trough of the Valles Marineris, a rift system that belongs to the Tharsis region of Mars. The ILD investigated is characterized by spectral signatures of kieserite, an evaporitic mineral present on Earth. A morphologic and morphometric survey of the ILD surface performed on data of the Orbiter High Resolution Imaging Science Experiment (HiRISE) highlighted the presence of depressions of various shapes and sizes. These landforms interpreted as dolines resemble similar karst landforms on Earth and in other regions of Mars. The observed karst landforms suggest the presence of liquid water, probably due to ice melting, in the Amazonian age. Keywords: Mars, interior layered deposits, karst, climate change Received 21 Octomber 2016; Revised 18 April 2017; Accepted 19 April 2017 Citation: Baioni D. and Tramontana M., 2017. Possible evaporite karst in an interior layered deposit in Juventae Chasma, Mars. International Journal of Speleology, 46 (2), 181-189. Tampa, FL (USA) ISSN 0392-6672 https://doi.org/10.5038/1827-806X.46.2.2085 INTRODUCTION north of Valles Marineris (Catling et al., 2006). -
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