ALTERATION on MARS: the VIEW from ORBIT 6:00 P.M
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Evidence for Volcanism in and Near the Chaotic Terrains East of Valles Marineris, Mars
43rd Lunar and Planetary Science Conference (2012) 1057.pdf EVIDENCE FOR VOLCANISM IN AND NEAR THE CHAOTIC TERRAINS EAST OF VALLES MARINERIS, MARS. Tanya N. Harrison, Malin Space Science Systems ([email protected]; P.O. Box 910148, San Diego, CA 92191). Introduction: Martian chaotic terrain was first de- ple chaotic regions are visible in CTX images (Figs. scribed by [1] from Mariner 6 and 7 data as a “rough, 1,2). These fractures have widened since the formation irregular complex of short ridges, knobs, and irregular- of the flows. The flows overtop and/or bank up upon ly shaped troughs and depressions,” attributing this pre-existing topography such as crater ejecta blankets morphology to subsidence and suggesting volcanism (Fig. 2c). Flows are also observed originating from as a possible cause. McCauley et al. [2], who were the fractures within some craters in the vicinity of the cha- first to note the presence of large outflow channels that os regions. Potential lava flows are observed on a por- appeared to originate from the chaotic terrains in Mar- tion of the floor as Hydaspis Chaos, possibly associat- iner 9 data, proposed localized geothermal melting ed with fissures on the chaos floor. As in Hydraotes, followed by catastrophic release as the formation these flows bank up against blocks on the chaos floor, mechanism of chaotic terrain. Variants of this model implying that if the flows are volcanic in origin, the have subsequently been detailed by a number of au- volcanism occurred after the formation of Hydaspis thors [e.g. 3,4,5]. Meresse et al. -
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. -
Aqueous Minerals from Arsia Chasmata of Arsia Mons, Tharsis Region: Implications for Aqueous Alteration Processes on Mars
45th Lunar and Planetary Science Conference (2014) 1826.pdf AQUEOUS MINERALS FROM ARSIA CHASMATA OF ARSIA MONS, THARSIS REGION: IMPLICATIONS FOR AQUEOUS ALTERATION PROCESSES ON MARS. N. Jain*, S. Bhattacharya, P. Chauhan, Space Applications Centre (ISRO), Ahmedabad, Gujarat, India ([email protected]/ Fax: +91-079- 26915825). Introduction: The Arsia Chasmata is a complex help of high resolution data such as MGS-MOC (Mars collapsed region located at the northeastern flank of Global Surveyor-Mars Orbiter Camera), Viking orbiter Arsia Mons (figure 1 A and B) within Tharsis region [3], fresh appearing lava flows [4], graben and glaciers of planet Mars and is the most important region for the on flanks of Arsia Mons [5], young lava flows [6] study of minerals like phyllosilicate and pyroxene. The small shields at floor of caldera [7]. reflectance data of MRO-CRISM (figure 1 C D) has Present study mainly focuses on the mineralogy of confirmed above mentioned minerals in the study area. Arsia Chasmata which interestingly contains The presence of these minerals at the Arsia Chasmata absorption features of aqueous altered minerals such as on Mars provides the evidence of its past watery serpentine (phyllosilicate). This mineral is also located environment and their processes of formation. In the in Nili Fossae region which is long, narrow depression present study the absorption features of serpentine present on Mars [8]. But in the present study (phyllosilicate) are obtained at 2.32 µm, 1.94 µm and occurrence of this mineral at high altitude region raise 2.51 µm. Previous studies on Mars show that the curiosity to know about their formation processes. -
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. -
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. -
An Overview of Morphological and Compositional Investigation of Melas Chasma of Valles Marineris
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6145.pdf An Overview of Morphological and Compositional investigation of Melas Chasma of Valles Marineris. T. Sivasankari1 and S. Arivazhagan2, 1 2 Centre For Applied Geology, Gandhigram Rural Institute - Deemed to be University, Gandhigram, Dindigul-624302, India ([email protected] and [email protected]). Introduction Many studies had been carried out by the primarily by aeolian processes in the recent period of time. researchers for various region of Valles Marineris and has Fig. 2. Shows the geology map of the study area. The geolo- revealed evidence for the presence of sulphate deposits gy map of Melas chasma was derived based on the map giv- namely the Interior Layered Deposits (ILD). The present en by Witbeck et al, 1991. The geological features includes study aims at the identification of mafic minerals High Cal- slope materials on the valley walls, dunes, layered materials, cium Pyroxene [HCP] and Phyllosilicate minerals of Melas fractured sediments, ridged plains, floor materials and crater chasma region of Valles Marineris by using CRISM datasets. fill materials. The topography of Chasma was interpreted by The spectra and the mineral distribution maps are derived the contuor map and DEM derived using the MOLA data. using the spectral summary parameters which helps to under- The contour values shows the highest relief of the study area stand the past geologic events ultimately bringing out the is 4000m and the lowest relief is -3800m. From the DEM origin and evolution of Valles Marineris. The Morphological data it is evident that the chasma has almost smooth valley features of Valles Marineris are compared with the CRISM floor with small isolated patches and a rugged topography as well as the HiRiSE Data. -
KILOMETER-SIZED CONES on MARS: IGNEOUS OR MUD VOLCANOES?. P. Brož1, P. Fawdon2, and O. Čadek3, 1Institute of Geophysics Of
Lunar and Planetary Science XLVIII (2017) 1425.pdf KILOMETER-SIZED CONES ON MARS: IGNEOUS OR MUD VOLCANOES?. P. Brož1, P. Fawdon2, and O. Čadek3, 1Institute of Geophysics of the Czech Academy of Science ([email protected]), 2Birkbeck, University of London, Malet St, London WC1E 7HX, 3Faculty of Mathematics and Physics, Department of Geophysics, Charles University in Prague, Czech Republic. Introduction: There is an ongoing debate within scientific community about the formation process of kilometer-sized cones reported from several regions on Mars (e.g., [1-8]). Two of the main mechanisms con- sidered as possible explanations, are (1) small scale igneous volcanism (e.g., [1,4-7]) and (2) mud volcan- ism (e.g., [2,8,10]). It is important to differentiate be- tween these two processes because of the very different implications these processes have for the Martian crust and near surface environment. Small scale igneous activity implies Mars producing magma away from the large Amazonian volcanic centers, whereas mud vol- canism implies pressurized and mobile ground water in the past. Both processes involve key factors of envi- ronmental habitability meaning that understanding the origin of these features is important in our understand- ing of recent habitability of Mars. On Earth small volcanoes and mud volcanism form of morphologically similar landforms (Fig. 1). Both processes form cones with relatively steep flanks and central craters on their tops; often additionally associ- ated with flow-like units spreading around those cones. Consequently, because of this convergence of form, is not readily apparent how to distinguish between these two processes using satellite images. -
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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. -
Cambridge University Press 978-1-107-03629-1 — the Atlas of Mars Kenneth S
Cambridge University Press 978-1-107-03629-1 — The Atlas of Mars Kenneth S. Coles, Kenneth L. Tanaka, Philip R. Christensen Index More Information Index Note: page numbers in italic indicates figures or tables Acheron Fossae 76, 76–77 cuesta 167, 169 Hadriacus Cavi 183 orbit 1 Acidalia Mensa 86, 87 Curiosity 9, 32, 62, 195 Hadriacus Palus 183, 184–185 surface gravity 1, 13 aeolian, See wind; dunes Cyane Catena 82 Hecates Tholus 102, 103 Mars 3 spacecraft 6, 201–202 Aeolis Dorsa 197 Hellas 30, 30, 53 Mars Atmosphere and Volatile Evolution (MAVEN) 9 Aeolis Mons, See Mount Sharp Dao Vallis 227 Hellas Montes 225 Mars Chart 1 Alba Mons 80, 81 datum (zero elevation) 2 Hellas Planitia 220, 220, 226, 227 Mars Exploration Rovers (MER), See Spirit, Opportunity albedo 4, 5,6,10, 56, 139 deformation 220, See also contraction, extension, faults, hematite 61, 130, 173 Mars Express 9 alluvial deposits 62, 195, 197, See also fluvial deposits grabens spherules 61,61 Mars Global Surveyor (MGS) 9 Amazonian Period, history of 50–51, 59 Deimos 62, 246, 246 Henry crater 135, 135 Mars Odyssey (MO) 9 Amenthes Planum 143, 143 deltas 174, 175, 195 Herschel crater 188, 189 Mars Orbiter Mission (MOM) 9 Apollinaris Mons 195, 195 dikes, igneous 82, 105, 155 Hesperia Planum 188–189 Mars Pathfinder 9, 31, 36, 60,60 Aram Chaos 130, 131 domical mound 135, 182, 195 Hesperian Period, history of 50, 188 Mars Reconnaissance Orbiter (MRO) 9 Ares Vallis 129, 130 Dorsa Argentea 239, 240 Huygens crater 183, 185 massif 182, 224 Argyre Planitia 213 dunes 56, 57,69–70, 71, 168, 185, -
Briony H. N. Horgan
December 2019 Briony H. N. Horgan 550 Stadium Mall Drive, West Lafayette, IN 47907 Assistant Professor [email protected] Department of Earth, Atmospheric, and Planetary Sciences (503) 703-8473 & School of Aeronautics and Astronautics Purdue University Education and Appointments 2014-present Assistant Professor, Purdue University 2013 Faculty Research Associate, Arizona State University 2010-2012 Exploration Postdoctoral Fellow, Arizona State University Advisor: Prof. Phil Christensen 2005-2010 Ph.D., Cornell University, Astronomy and Space Sciences Advisor: Prof. Jim Bell 2001-2005 B.S., Oregon State University, Physics, summa cum laude Fields of Expertise • Surface geology, mineralogy, rover studies, and remote sensing of the terrestrial planets • Visible, near-infrared, and thermal-infrared spectroscopy • Mapping and analysis of large hyperspectral datasets • Planetary analog field studies of weathering, aeolian, volcanic, and glacial processes NASA Mission Experience 2016-present Participating Scientist, Mars Science Laboratory Mission 2015-present Co-I, Mastcam-Z imaging investigation, Mars2020 Mission 2008-2014 Science Team, THEMIS, Mars Odyssey Mission Support: Current and Past 2021-2024 Co-Investigator, NASA Solar Systems Working Program Between a rock and a frozen place: Cold-based glacial chemical alteration of volcanic bedrock as an analog for Mars (PI: Dr. Alicia Rutledge) 2020-2021 Co-Investigator, NASA Planetary Mission Concepts Studies Mars Orbiter for Resources, Ice, and Environment (PI: Prof. Wendy Calvin) 2020-2023 Co-Investigator, NASA Mars2020 Mission Phase E Mastcam-Z: A Geologic, Stereoscopic, and Multispectral Investigation for the NASA Mars 2020 Rover Mission (PI: Prof. Jim Bell) 2020-2023 Co-Investigator, NASA Lunar Data Analysis Program Investigating Explosive Volcanic Deposits in the Montes Apenninus area using Moon Mineralogy Mapper Data (PI: Dr.