DOCSLIB.ORG

Igneous Compositions in Ares Vallis: Timing and Importance of Volcanics and Fluvial Processes at the Noachian-Hesperian Boundary

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Igneous Compositions in Ares Vallis: Timing and Importance of Volcanics and Fluvial Processes at the Noachian-Hesperian Boundary 42nd Lunar and Planetary Science Conference (2011) 2507.pdf IGNEOUS COMPOSITIONS IN ARES VALLIS: TIMING AND IMPORTANCE OF VOLCANICS AND FLUVIAL PROCESSES AT THE NOACHIAN-HESPERIAN BOUNDARY. J. H. Wilson1 and J. F. Mustard1, 1Department of Geological Sciences, Brown University, Providence, RI 02912 ([email protected]) Introduction: Ares Vallis is one of many outflow mented as described in [22]. Both the L and S detector channels on Mars generally thought to have formed by data were used. We will be using the much improved the catastrophic outflow of subsurface water e.g. [1, 2, TRR3 data formation as they becom available but this 3]. Yet, the presence of diagnostic signatures of igne- research is focused on the starndard TRR2 data. Spec- ous compositions indicates a complex history. Olivine tra were extracted from regions of interest on the basis is one of the more readily detected igneous mineral of spectral parameter maps [23] using a 5 X 5 pixel signatures and has been detected globally with various average. Residual artifacts after calibration and atmos- instruments including TES, e.g. [4, 5, 6, 7, 8], pheric removal are suppressed by ratioing the spectra THEMIS, e.g. [4, 8, 9], OMEGA, e.g. [10, 11, 12], and to a spectrally neutral region from the same column by the MER rovers in situ, e.g. [13, 14, 15]. Deposits because of the nature of 2-D detectors. with igneous signatures in Ares Vallis can be detected CTX and HiRISE observations, P07_003762_1861 with the high resolution Compact Reconnaissance Im- and ESP_013216_1870 and PSP_008166_1885, re- aging Spectrometer for Mars (CRISM) [16] and their spectively, were used to document morphologies. An morphologic and geologic context assessed with the ArcGIS-ready MOLA [24] raster from the USGS was Context Camera (CTX) [17], the High Resolution Im- used to aid in the interpretation of the morphologies. aging Science Experiment (HiRISE) [18] data, as well Mineral Detections: Mafic minerals are recog- as other imaging sensors, allowing for a more detailed nized and mapped on the basis of crystal field transi- characterization of the deposits. tion absorptions in the 1-2.5 µm region and procedures Ares Vallis has been proposed to have been formed for this recognition and mapping have been presented by multiple outflow events; crater counting in the area previously [12, 22]. Olivine and pyroxene have been has dated the exposed surface of Ares Vallis at an age detected on the floor of Ares Vallis, whereas only oli- of mid-Hesperian e.g. [19] or Hesperian to early Ama- vine detections have been made on the plateau to the zonian e.g. [20]. In addition, data from instruments on east of the channel and on the edges of the channel, the Mars Reconnaissance Orbiter (MRO) and Mars near the outflow source (Fig. 1). Olivine is recognized Express allow the characterization of the nature of the by its broad 1 µm absorption, while pyroxene is recog- Noachian plains units between Ares Vallis and Meri- nized by its broad 1 and 2 µm absorptions. The pyrox- diani Planum. In light of these findings, it is of interest ene absorptions indicate a composition intermediate to constrain the timing of igneous, volcanic and fluvial between low-Ca (LCP) and high-Ca (HCP) and resem- activity in the area. In particular, Ares Valles formed bles spectra of Hawaiian basalt, from the CRISM spec- at the critical period near the stratigraphic boundary tral library [25]. Since LCP-rich compositions are more between the Noachian and Hesperian as global-scale common in old Noachian terrains and more HCP-rich processes transitioned from the era of phyllosilicate in Hesperian terrains [12, 26], it is possible that the formation to sulfate formation [21]. lava flow in the floor of Ares Vallis has captured a shift Datasets and Methods: We use data from the Ob- in the evolution of magmas. Olivines on the plains servatoire pour la Minéralogie, l'Eau, les Glaces, et units are similar in spectral character to those of Noa- l'Activité [21]. Basic reduction of OMEGA data from chian olivines in the Nili Fossae region and have no radiance to reflectance including atmospheric removal detectable pyroxene absoprtions. The deposits on the is performed as described by [12]. We also analyze full channel floor are clearly of a different nature than those resolution CRISM TRR2 observations that cover parts found on the surrounding, geologically older plateaus. of the floor of Ares Vallis in the vicinity of 6.7°N, Morphology: HiRISE shows that the deposits on 19.5W, as well as some of the surrounding terrains. the floor of Ares Vallis, where mafic detections are These are full resolution targeted hyperspectral obser- observed with CRISM, have a texture analagous to vations with spatial resolutions of 18-36 meters per cooling fractures in lava (Figs. 1a,b,c). [27] has re- pixel in 544 separate wavelengths between 0.362 μm ported olivine signatures in floor deposits and ejecta and 3.92 μm in hyperspectral mode with a spectral res- associated with Taytay crater on the northeastern edge olution of 6.55 nm/channel. CRISM multispectral data of Ares Vallis. The spectra from the central peaks ex- available over the plains units consist of a subset of 72 hibit weak Fe/Mg phyllosilicate absorptions suggesting wavelengths binned to 200 meters per pixel. The at- excavation of Noachian basement; Taytay is large mospheric and photometric corrections were imple- enough to excavate to a depth [28] comparable to that 42nd Lunar and Planetary Science Conference (2011) 2507.pdf of the channel floor’s current elevation. Furthermore, rian-aged lava flow on the floor of Ares Vallis may the ejecta of Taytay crater cover this mafic deposit in capture a compositional evolution in this region. Since the channel. These observations, together, are indica- the detections herein are similar to other Hesperian tive that the mafic unit, dated to the early Hesperian volcanics, this regional compositional evolution may [29], that forms the floor of the channel is a post- be important for interpreting igneous materials from channel fill that occurred sometime before or during other regions on Mars. the early Hesperian (Fig. 1c). Future Work: Crater counts will be performed on MOLA topography profiles indicate that the floor the plateau units that appear to be resurfacing events, in of Ares Vallis is very flat and that it slopes downward order to determine their relationship to the Noachian from both ends to a point near the bend in the channel basement and for. The derived ages will then be relata- at 10°N, 23.9°W. HiRISE and CTX show that the ble to the ages given by other authors for Ares Vallis. floor deposit in this region covers previously carved References: [1] Carr, M. H. (1979) JGR 84, 2995-3007. [2] terraces in the wall of the channel; therefore the mafic Baker, V. R. (1982) University of Texas Press, Austin, 198 pp. [3] fill was emplaced after the channel was formed and is Baker, V. R. et al. (1992) University of Arizona Press, Tucson, 493- 522. [4] Rogers A. D. et al. (2005) JGR, 110, E05010. [5] Hoefen T. not simply mafic rock exposed by fluvial erosion. M. et al. (2003) Science, 302, 627-630. [6] Bandfield J. L. (2002) Conclusions: It is clear from morphology and JGR,107(E6), 5042. [7] Hamilton V. E. et al. (2003) Meteorit. Pla- spectral characteristics that Taytay crater does not con- net. Sci., 38, 871-885. [8] Koeppen W. C. and Hamilton V. E. tain detectable pyroxene and that it does not excavate (2008) JGR, 113, E05001. [9] Hamilton V. E. and Christiansen P. R. (2005) Geology, 33, 433-436. [10] Bibring J. P. (2005) Science, the same layer of mafic material that is present on the 307, 5715, 1576-1581. [11] J. F. Mustard et al., Science 307, 5715, floor of Ares Vallis. The spectra of the deposit on the 1594-1597, 2005. [12] Poulet F. (2007) JGR, 112, E08S02. [13] floor of Ares Vallis are consistent with Hesperian lava Christensen P. R. et al. (2004b) Science, 306, 1733-1739. [14] flows elsewhere [26, 30]. The source of the volcanics McSween H. Y. Jr. et al. (2004) Science, 305, 842-845. [15] Morris R. V. et al. (2004) Science, 305, 833-836. [16] Murchie S. et al. on the floor of Ares Vallis is not clear: a potential vol- (2007) JGR, 112, E05S03. [17] Malin M. C. et al. (2007) JGR, 112, canic cone is present in the floor of Ares Vallis and this E05S04. [18] McEwen A. S. et al. (2007) JGR, 112, E05S02. [19] may be their source (Fig. 1b); however, it is apparent Costard F. and Baker V. R. (2001)Geomorphology, 37, 3-4, pp.289- that the lava could not have come from the northern 301. [20] Warner W.H. et al. (2010) Geology, 38, 9, p.791–794. [21] Bibring J.P. et al. (2006) Science 312, 400. [22] Mustard J. F. plains given the present topography (Fig. 1d). The et al. (2008) Nature, 454, 305. [23] Pelkey S.M. et al. (2007) JGR, morphologic relationships regarding the ejecta from 112, E08S14 [24] Smith D. E. et al. (2001) JGR, 106, 23,689– Taytay crater and the mafic floor deposit confirm the 23,722. [25] Murchie, S. et al. (2006) NASA PDS MRO-M-CRISM- current hypothesis that most outflow occurred early in 4-SPECLIB-v1.0. [26] Skok J.R. et al. (2010) JGR, 115, E00D14. Mars’ history, by the end of the Noachian, and that [27] Wilson J.H. and Mustard J.F. (2010) LPSC XLI,abstract 2516.
Load more

Recommended publications
  • Salt Triggered Melting of Permafrost in the Chaos Regions of Mars
    Lunar and Planetary Science XXXVII (2006) 2218.pdf SALT TRIGGERED MELTING OF PERMAFROST IN THE CHAOS REGIONS OF MARS. Popa I.C., Università degli Studi "G. d'Annunzio" Chieti-Pescara, Pescara, Viale Pindaro 42, Italy. ([email protected]) Introduction: Mars surface bears traces of many landing site (Chryse Planitia) is the place where Ares fluvial-like features, geomorphic identified as outflow outflow channel is depositing its transporting channels, valley networks etc. Among these a particular materials. The following Martian landers Pathfinder one stands above others from the dimensional point of [6] and MER A Spirit [7], and MER B Opportunity [8] view. Outflow channels bear unique water erosion also revealed high soluble salts contents in places characteristics, that led Baker and Milton (1974) [1] to possibly genetically connected. Recently OMEGA believe that are caused by a surface runoff of large aboard Mars Express spacecraft has proven the amounts of water, in short geological time. Water existence of gypsum and other highly soluble salts (e.g origin, necessary for these processes was the topic of kieserite and epsomite) in localized deposits in places around Valles Marineris, and Iani Chaos [9]. many works. Among these theories one generally Freezing point depression of water solutions: accepted idea considers that water is originating from The freezing point of pure water at 1 bar is 0°C melting of permafrost layers positioned in the places of (273K). This melting point can be easily depressed by today chaos’. Here is an investigation that takes into adding impurities or soluble salts to the solvent. In the account the exoergic salt-ice dissolution reaction, along case of halite (NaCl) salt it is known that a 10% NaCl with freezing point depression of formed salty solutions, solution lowers the melting point of about -6°C (267K) as a complentary or a stand-alone process in chaos- and a 20% salt solution lowers it to -16°C (257K).
    [Show full text]
  • Download Student Activities Objects from the Area Around Its Orbit, Called Its Orbital Zone; at Amnh.Org/Worlds-Beyond-Earth-Educators
    INSIDE Essential Questions Synopsis Missions Come Prepared Checklist Correlation to Standards Connections to Other Halls Glossary ONLINE Student Activities Additional Resources amnh.org/worlds-beyond-earth-educators EssentialEssential Questions Questions What is the solar system? In the 20th century, humans began leaving Earth. NASA’s Our solar system consists of our star—the Sun—and all the Apollo space program was the first to land humans on billions of objects that orbit it. These objects, which are bound another world, carrying 12 human astronauts to the Moon’s to the Sun by gravity, include the eight planets—Mercury, surface. Since then we’ve sent our proxies—robots—on Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune; missions near and far across our solar system. Flyby several dwarf planets, including Ceres and Pluto; hundreds missions allow limited glimpses; orbiters survey surfaces; of moons orbiting the planets and other bodies, including landers get a close-up understanding of their landing Jupiter’s four major moons and Saturn’s seven, and, of course, location; and rovers, like human explorers, set off across the Earth’s own moon, the Moon; thousands of comets; millions surface to see what they can find and analyze. of asteroids; and billions of icy objects beyond Neptune. The solar system is shaped like a gigantic disk with the Sun at The results of these explorations are often surprising. With its center. Everywhere we look throughout the universe we the Moon as our only reference, we expected other worlds see similar disk-shaped systems bound together by gravity. to be cold, dry, dead places, but exploration has revealed Examples include faraway galaxies, planetary systems astonishing variety in our solar system.
    [Show full text]
  • The Periglacial Landscape of Utopia Planitia; Geologic Evidence for Recent Climate Change on Mars
    Western University Scholarship@Western Electronic Thesis and Dissertation Repository 1-23-2013 12:00 AM The Periglacial Landscape Of Utopia Planitia; Geologic Evidence For Recent Climate Change On Mars. Mary C. Kerrigan The University of Western Ontario Supervisor Dr. Marco Van De Wiel The University of Western Ontario Joint Supervisor Dr. Gordon R Osinski The University of Western Ontario Graduate Program in Geography A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Mary C. Kerrigan 2013 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Climate Commons, Geology Commons, Geomorphology Commons, and the Physical and Environmental Geography Commons Recommended Citation Kerrigan, Mary C., "The Periglacial Landscape Of Utopia Planitia; Geologic Evidence For Recent Climate Change On Mars." (2013). Electronic Thesis and Dissertation Repository. 1101. https://ir.lib.uwo.ca/etd/1101 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. THE PERIGLACIAL LANDSCAPE OF UTOPIA PLANITIA; GEOLOGIC EVIDENCE FOR RECENT CLIMATE CHANGE ON MARS by Mary C. Kerrigan Graduate Program in Geography A thesis submitted in partial fulfillment of the requirements for the degree of Master of Science The School of Graduate and Postdoctoral Studies The University of Western Ontario London, Ontario, Canada © Mary C. Kerrigan 2013 ii THE UNIVERSITY OF WESTERN ONTARIO School of Graduate and Postdoctoral Studies CERTIFICATE OF EXAMINATION Joint Supervisor Examiners ______________________________ Dr.
    [Show full text]
  • Program Lists the Abstracts for All Submissions for GREAT Day(S) 2021
    the 15th annual virtual monday april 26, 2021 - friday april 30, 2021 geneseo recognizing excellence, achievement, and talent th 2021 Geneseo Recognizing Excellence Achievement and Talent Day • 15 Annual Welcome to SUNY Geneseo’s Fifteenth Annual GREAT Day(s)! Geneseo Recognizing Excellence, Achievement & Talent Day is a college-wide symposium celebrating the creative and scholarly endeavors of our students. In addition to recognizing the achievements of our students, the purpose of GREAT Day is to help foster academic excellence, encourage professional development, and build connections within the community. http://www.geneseo.edu/great_day This program lists the abstracts for all submissions for GREAT Day(s) 2021. Due to the COVID-19 pandemic, GREAT Day(s) 2021 is happening virtually and will be held during the week of April 26th – April 30th. The keynote address by Dr. Adam Frank will be held synchronously on Wednesday, April 28th at 2:30 PM. Scholarly and creative projects in a variety of formats will be available for viewing beginning April 26th. To view presentations, check the Virtual Program on the GREAT Day webpage at: http://www.geneseo.edu/great_day GREAT Day often falls on or near Earth Day, which is held on April 22nd each year. In recognition of this, presentations that have been self- identified by students as promoting sustainability are designated by a leaf symbol - - in this program. Throughout the day, when you post about GREAT Day(s) on social media use #WeAreGREAT to be featured on GREAT Day social media! GreatDayGeneseo @GeneseoGREATDay geneseo.edu/great_day 2 2021 Geneseo Recognizing Excellence Achievement and Talent Day • 15th Annual Honors TABLE OF CONTENTS Program reflects updates as of April 25, 2021 GREAT Day Honors ...................................................................................................................
    [Show full text]
  • Near-Surface Geologic Units Exposed Along Ares Vallis and in Adjacent Areas: a Potential Source of Sediment at the Mars Oz C
    https://ntrs.nasa.gov/search.jsp?R=19970022395 2020-06-16T02:32:22+00:00Z View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by NASA Technical Reports Server NASA-CR-206.689 JOURNAL UI" ut_t .... _CAL RESEARCH, VOL. 102,NO. E2, PAGES 4219-4229, FEBRUARY 25, 1997 Near-surface geologic units exposed along Ares Vallis and in adjacent areas: A potential source of sediment at the Mars Oz C_. <-- Pathfinder landing site Allan H. Treiman Lunar and Planetary Institute, Houston,Texas Abstract. A sequence of layers, bright and dark, is exposed on the walls of canyons, impact craters and mesas throughout the Ares Vallis region, Chryse Planitia, and Xanthe Terra, Mars. Four layers can be seen: two pairs of alternating dark and bright albedo. The upper dark layer forms the top surface of many walls and mesas. The upper dark- bright pair was stripped as a unit from many streamlined mesas and from the walls of Ares Valles, leaving a bench at the top of the lower dark layer, "250 m below the highland surface on streamlined islands and on the walls of Ares Vallis itself. Along Ares Vallis, the scarp between the highlands surface and this bench is commonly angular in plan view (not smoothly curving), suggesting that erosion of the upper dark-bright pair of layers controlled by planes of weakness, like fractures or joints. These near-surface layers in the Ares Vallis area have similar thicknesses, colors, and resistances to erosion to layers exposed near the tops of walls in Valles Marineris [Treiman et al., 1995] and may represent the same pedogenic hardpan units.
    [Show full text]
  • Mars Pathfinder Landing Site Workshop Ii: Characteristics of the Ares Vallis Region and Field Trips in the Channeled Scabland, Washington
    /, NASA-CR-200508 L / MARS PATHFINDER LANDING SITE WORKSHOP II: CHARACTERISTICS OF THE ARES VALLIS REGION AND FIELD TRIPS IN THE CHANNELED SCABLAND, WASHINGTON LPI Technical Report Number 95-01, Part 1 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI/TR--95-01, Part 1 "lp MARS PATHFINDER LANDING SITE WORKSHOP II: CHARACTERISTICS OF THE ARES VALLIS REGION AND FIELD TRIPS IN THE CHANNELED SCABLAND, WASHINGTON Edited by M. P. Golombek, K. S. Edgett, and J. W. Rice Jr. Held at Spokane, Washington September 24-30, 1995 Sponsored by Arizona State University Jet Propulsion Laboratory Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 95-01, Part 1 LPI/TR--95-01, Part 1 Compiled in 1995 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the University Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may he 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 he cited as Golomhek M. P., Edger K. S., and Rice J. W. Jr., eds. ( 1992)Mars Pathfinder Landing Site Workshop 11: Characteristics of the Ares Vallis Region and Field Trips to the Channeled Scabland, Washington. LPI Tech. Rpt. 95-01, Part 1, Lunar and Planetary Institute, Houston. 63 pp.
    [Show full text]
  • The GEAS Project: Astronomy Laboratory
    Lab 4 Cratering and the Martian Surface 4.1 Introduction Human space travel enthusiasts hope that our manned missions to the Moon will serve as stepping stones for an eventual trip to Mars. Our “visit” to the Moon in our previous lunar cratering laboratory exercise has prepared us similarly to visit Mars today. We have already learned that cratering is a key process in shaping the appearance of terrestrial planetary surfaces, and that counting craters can help determine the ages of surface features. We studied techniques used to decide which geological event occurred first, or which surface is younger (relative dating techniques), and also learned how to determine absolute ages based on radioactive dating of physical samples. Lunar and Martian surfaces are similar in many ways (both types are heavily cratered in some places and covered with smooth ancient lava flows in others), but they exhibit several important differences. First, volcanic features on Mars are much more prominent than those on the Moon. Mars has the largest volcanoes in the entire solar system, and some of them have clearly become inactive only recently. (Some planetary scientists suspect that the largest Martian volcano of all, Olympus Mons, may still be active today.) Second, unlike the bone-dry Moon, Mars was once a very wet planet. Its surface contains channel and river delta-like features that were undeniably formed by flowing water in the past. These differences lead us to two important questions. When did the last volcanic eruptions occur on Mars, and when did water last flow freely there? In this lab, you’ll use crater counting techniques to help reconstruct a Martian surface chronology and investigate these questions.
    [Show full text]
  • Modern Mars' Geomorphological Activity
    Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, Matthew Chojnacki, Susan Conway, Colin Dundas, Candice Hansen, Alfred Mcewen, et al. To cite this version: Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, et al.. Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity. Geomorphology, Elsevier, 2021, 380, pp.107627. 10.1016/j.geomorph.2021.107627. hal-03186543 HAL Id: hal-03186543 https://hal.archives-ouvertes.fr/hal-03186543 Submitted on 31 Mar 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 Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity 2 3 Authors: Serina Diniega1,*, Ali M. Bramson2, Bonnie Buratti1, Peter Buhler3, Devon M. Burr4, 4 Matthew Chojnacki3, Susan J. Conway5, Colin M. Dundas6, Candice J. Hansen3, Alfred S. 5 McEwen7, Mathieu G. A. Lapôtre8, Joseph Levy9, Lauren Mc Keown10, Sylvain Piqueux1, 6 Ganna Portyankina11, Christy Swann12, Timothy N. Titus6,
    [Show full text]
  • Tuesday, March 22, 2016 [T319] POSTER SESSION I: MARTIAN MINERALOGY from ORBIT and on the SURFACE 6:00 P.M
    47th Lunar and Planetary Science Conference (2016) sess319.pdf Tuesday, March 22, 2016 [T319] POSTER SESSION I: MARTIAN MINERALOGY FROM ORBIT AND ON THE SURFACE 6:00 p.m. Town Center Exhibit Area Clark R. N. Swayze G. A. Murchie S. L. Seelos F. P. Viviano-Beck C. E. et al. POSTER LOCATION #291 Mapping Water and Water-Bearing Minerals on Mars with CRISM [#2900] We have analyzed over 200 CRISM scenes, and find diverse signatures of water using the 2-micron absorption. Seelos F. P. Viviano-Beck C. E. Morgan M. F. Romeo G. Aiello J. J. et al. POSTER LOCATION #292 CRISM Hyperspectral Targeted Observation PDS Product Sets — TERs and MTRDRs [#1783] Targeted Empirical Records (TERs) and Map-projected Targeted Reduced Data Records (MTRDRs) — High level CRISM targeted observation data product sets. Pan C. Rogers A. D. POSTER LOCATION #293 Olivine-Rich Basalt Outcrops in the Subsurface of Western Noachis Terra, Mars, and Geological Implications [#1528] Olivine-rich outcrops found in Ladoon Valles and Uzboi Vallis, suggesting they may be widespread and form a continuous unit in Valles Marineris and Ares Vallis. Brown A. J. Viviano-Beck C. E. Bishop J. L. Cabrol N. A. Andersen D. et al. POSTER LOCATION #294 A Serpentinization Origin for Jezero Crater Carbonates [#2165] Using CRISM, we investigated spectral signatures of carbonates in Jezero Crater and conclude they are more like Nili Fossae brethren than previously suspected. Jain N. S. Chauhan P. Rajashekhar P. POSTER LOCATION #295 Evidences of Aqueous past of Ladon Valles Region on Mars Through Morphology and Mineralogy [#1114] Mineralogy, geomorphology and morphometric analysis of Ladon valleys, Mars.
    [Show full text]
  • In Ares Vallis
    Mars Express: Current flows and 'islands' in Ares Vallis 07 October 2011 The Ares Vallis outflow channel meanders for more than 1700 kilometres across the southern highlands of Mars and ends in a 100-kilometre-wide delta-like region in the lowlands of Chryse Planitia. On 11 May 2011, parts of the Ares Vallis channel were photographed using the High Resolution Stereo Camera (HRSC) operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) on board ESA's Mars Express spacecraft during orbit 9393. The images show a large, partially eroded crater, streamlined 'islands' and terrace-like 'river banks' on the valley walls; all signs of erosion by the water that, in the period of Mars’ early formation, would have flowed through Ares Vallis. The photographs, acquired from an altitude of 300 kilometres, show a section of the Ares Vallis channel located at 16 degrees north and 327 degrees east. The image resolution is about 15 metres per pixel. The valley was named after Ares, the Greek god of war, whose counterpart among the Roman deities was Mars. The Ares Vallis outflow channel was discovered in 1976 in images acquired by the US Viking spacecraft. In 1997, the small Mars Pathfinder rover landed in the Ares Vallis channel to investigate the signs of water flow. The most distinctive landscape characteristic is the large impact crater Oraibi, about 32 kilometres across. The crater lies just 100 kilometres south of where Pathfinder landed (see context map) on 4 July 1997; it explored the area for 12 weeks. Crater flooded by large quantities of water The signs of erosion are easily spotted on the Oraibi crater.
    [Show full text]
  • Ganges Chasma Sand Sheet: Science at a Proposed “Safe” Mars Landing Site
    GANGES CHASMA SAND SHEET: SCIENCE AT A PROPOSED “SAFE” MARS LANDING SITE. K. S. Edgett, Malin Space Science Systems, P.O. Box 910148, San Diego, CA 92191-0148, ([email protected]). Introduction: The only place within the elevation standing the nature of early Mars (e.g., aqueous sedi- and latitude constraints for the Mars Surveyor Project mentary origins are among those proposed). 2001 (MSP01) lander that is almost guaranteed to be safe for landing is the large, smooth, nearly flat sand Geologic Setting: Ganges Chasma is one of the sheet that covers much of the floor of Ganges Chasma. troughs of the Valles Marineris system. It is open to While at first it might seem that this kind of surface the east, and it appears to connect to the Hy- would be boring, an array of topics consistent with draotes/Simud Valles system. There is a notch in the Mars Surveyor goals can be addressed at this site. north wall of the chasm that appears to be related to subsurface collapse that connects to Shalbatana Vallis. Rationale: The reason I suggest landing on the On the upland west and south of Ganges Chasma, there smooth sand sheet in Ganges Chasma is very simple. are relatively small (for Mars) scoured valleys that re- It is safe. When it arrives, the MSP01 lander will have semble miniature outflow channels. Both of these ap- only ~31 cm of clearance with respect to obstacles such pear to have “drained” into Ganges Chasma at some as rocks. Mars Global Surveyor (MGS) Mars Orbiter time in the past.
    [Show full text]
  • The Nature of Remnant Mounds on the Margin of Chryse Planitia
    T h e N a t u re o f R e m n a n t M o u n d s o n t h e M a rg i n of Chryse Planitia ¹School of Physical Sciences, The Open University, Milton Keynes, UK Joe McNEIL¹ Matt BALME¹ Peter FAWDON¹ Angela COE² ²School of Environment, Earth and Ecosystem Sciences, The Open University, Milton Keynes, UK [email protected] @joseph_mcneil Abstract #1948 INTRODUCTION Figure 1 • There are thousands of kilometre-scale mounds distributed around the southern margin of Chryse Planitia, a ~1090 km diameter MOLA quasi-circular basin that lies north of the dichotomy boundary (Pan et al., 2019, Figure 1A-C). projection of study area and • Large numbers of mounds are present in Oxia Colles/Oxia Planum (Figure 1A), Hypanis Vallis (Figure 1B), and atop the Simud Valles sub-study areas MAWRTH / Ares Vallis channel islands (Figure 1C). C.P. IA STUDY AREA • Despite being a widespread geomorphological feature in this important highland-lowland transitional region, their origin VALLIS and stratigraphic position are poorly understood. 1A: OX • This study has investigated the morphology and distribution of these landforms in order to understand their place in the stratigraphy and their role in the geological history of the area. • Mounds have been identified and digitised using a combination of CTX, HRSC, and MOLA data, and classified based on their • M o u n d CSproportions morphologies. Heights have been determined from the intersection of their high and low points with individual MOLA shot data. Figure 2: MOLA globe showing global context of are extremely Chryse Planitia (C.P.), and the location of Figure 1.
    [Show full text]