Understanding Mars Through the Earth: Geochemical Characterization of Submarine Volcano Scenarios to Be Used As Martian Analogues
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Impact of High Temperatures on Aluminoceladonite Studied by Mössbauer, Raman, X-Ray Diffraction and X-Ray Photoelectron Spectroscopy
Title: Impact of high temperatures on aluminoceladonite studied by Mössbauer, Raman, X-ray diffraction and X-ray photoelectron spectroscopy Author: Mariola Kądziołka-Gaweł, Maria Czaja, Mateusz Dulski, Tomasz Krzykawski, Magdalena Szubka Citation style: Kądziołka-Gaweł Mariola, Czaja Maria, Dulski Mateusz, Krzykawski Tomasz, Szubka Magdalena. (2021). Impact of high temperatures on aluminoceladonite studied by Mössbauer, Raman, X-ray diffraction and X-ray photoelectron spectroscopy. “Mineralogy and Petrology” (Vol. 115, iss. 0, 2021, s. 1- 14), DOI: 10.1007/s00710-021-00753-z Mineralogy and Petrology (2021) 115:431–444 https://doi.org/10.1007/s00710-021-00753-z ORIGINAL PAPER Impact of high temperatures on aluminoceladonite studied by Mössbauer, Raman, X-ray diffraction and X-ray photoelectron spectroscopy Mariola Kądziołka-Gaweł1 & Maria Czaja2 & Mateusz Dulski3,4 & Tomasz Krzykawski2 & Magdalena Szubka1 Received: 9 March 2020 /Accepted: 28 April 2021 / Published online: 18 May 2021 # The Author(s) 2021 Abstract Mössbauer, Raman, X-ray diffraction and X-ray photoelectron spectroscopies were used to examine the effects of temperature on the structure of two aluminoceladonite samples. The process of oxidation of Fe2+ to Fe3+ ions started at about 350 °C for the sample richer in Al and at 300 °C for the sample somewhat lower Al-content. Mössbauer results show that this process may be associated with dehydroxylation or even initiate it. The first stage of dehydroxylation takes place at a temperature > 350 °C when the adjacent OH groups are replaced with a single residual oxygen atom. Up to ~500 °C, Fe ions do not migrate from cis- octahedra to trans-octahedra sites, but the coordination number of polyhedra changes from six to five. -
Wind-Eroded Stratigraphy on the Floor of a Noachian Impact Crater, Noachis Terra, Mars
Third Conference on Early Mars (2012) 7066.pdf WIND-ERODED STRATIGRAPHY ON THE FLOOR OF A NOACHIAN IMPACT CRATER, NOACHIS TERRA, MARS. R. P. Irwin III1,2, J. J. Wray3, T. A. Maxwell1, S. C. Mest2,4, and S. T. Hansen3, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, MRC 315, 6th St. at Independence Ave. SW, Washington DC 20013, [email protected], [email protected]. 2Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson AZ 85719, [email protected]. 3School of Earth and Atmospheric Sciences, Georgia Institute of Technology, 311 Ferst Drive, Atlanta GA 30332-0340, [email protected], [email protected]. 4Planetary Geodynamics Laboratory, Code 698, NASA Goddard Space Flight Center, Greenbelt MD 20771. Introduction: Detailed stratigraphic and spectral cular 12-km depression (a possible highly degraded studies of outcrops exposed in craters and other basins crater) on the southern side. The former received in- have significantly advanced the understanding of early ternal drainage from the north and east, whereas part Mars. Most studies have focused on high-relief sec- of the southern wall drained to the latter (Fig. 2). tions exposed by aeolian deflation, such as those in Gale crater, Arabia Terra, and Valles Marineris [1–3]. Many flat-floored Noachian degraded craters also have wind-eroded strata, suggesting that they lack a cap rock of Gusev-type basalts [4,5]. This study focuses on the youngest materials exposed on the wind-eroded floor of an unnamed Noachian degraded crater in Noachis Terra, Mars. The crater is centered at 20.2ºS, 42.6ºE and is 52 km in diameter. -
JUICE Red Book
ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat. -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
Washington State Minerals Checklist
Division of Geology and Earth Resources MS 47007; Olympia, WA 98504-7007 Washington State 360-902-1450; 360-902-1785 fax E-mail: [email protected] Website: http://www.dnr.wa.gov/geology Minerals Checklist Note: Mineral names in parentheses are the preferred species names. Compiled by Raymond Lasmanis o Acanthite o Arsenopalladinite o Bustamite o Clinohumite o Enstatite o Harmotome o Actinolite o Arsenopyrite o Bytownite o Clinoptilolite o Epidesmine (Stilbite) o Hastingsite o Adularia o Arsenosulvanite (Plagioclase) o Clinozoisite o Epidote o Hausmannite (Orthoclase) o Arsenpolybasite o Cairngorm (Quartz) o Cobaltite o Epistilbite o Hedenbergite o Aegirine o Astrophyllite o Calamine o Cochromite o Epsomite o Hedleyite o Aenigmatite o Atacamite (Hemimorphite) o Coffinite o Erionite o Hematite o Aeschynite o Atokite o Calaverite o Columbite o Erythrite o Hemimorphite o Agardite-Y o Augite o Calciohilairite (Ferrocolumbite) o Euchroite o Hercynite o Agate (Quartz) o Aurostibite o Calcite, see also o Conichalcite o Euxenite o Hessite o Aguilarite o Austinite Manganocalcite o Connellite o Euxenite-Y o Heulandite o Aktashite o Onyx o Copiapite o o Autunite o Fairchildite Hexahydrite o Alabandite o Caledonite o Copper o o Awaruite o Famatinite Hibschite o Albite o Cancrinite o Copper-zinc o o Axinite group o Fayalite Hillebrandite o Algodonite o Carnelian (Quartz) o Coquandite o o Azurite o Feldspar group Hisingerite o Allanite o Cassiterite o Cordierite o o Barite o Ferberite Hongshiite o Allanite-Ce o Catapleiite o Corrensite o o Bastnäsite -
Mineral Processing
Mineral Processing Foundations of theory and practice of minerallurgy 1st English edition JAN DRZYMALA, C. Eng., Ph.D., D.Sc. Member of the Polish Mineral Processing Society Wroclaw University of Technology 2007 Translation: J. Drzymala, A. Swatek Reviewer: A. Luszczkiewicz Published as supplied by the author ©Copyright by Jan Drzymala, Wroclaw 2007 Computer typesetting: Danuta Szyszka Cover design: Danuta Szyszka Cover photo: Sebastian Bożek Oficyna Wydawnicza Politechniki Wrocławskiej Wybrzeze Wyspianskiego 27 50-370 Wroclaw Any part of this publication can be used in any form by any means provided that the usage is acknowledged by the citation: Drzymala, J., Mineral Processing, Foundations of theory and practice of minerallurgy, Oficyna Wydawnicza PWr., 2007, www.ig.pwr.wroc.pl/minproc ISBN 978-83-7493-362-9 Contents Introduction ....................................................................................................................9 Part I Introduction to mineral processing .....................................................................13 1. From the Big Bang to mineral processing................................................................14 1.1. The formation of matter ...................................................................................14 1.2. Elementary particles.........................................................................................16 1.3. Molecules .........................................................................................................18 1.4. Solids................................................................................................................19 -
EROSION and BASIN MODIFICATION of SMALLER COMPLEX CRATERS in the ISIDIS REGION, MARS. J.A. Mclaughlin1 and A.K. Davatzes2, 1Temp
Lunar and Planetary Science XLVIII (2017) 1190.pdf EROSION AND BASIN MODIFICATION OF SMALLER COMPLEX CRATERS IN THE ISIDIS REGION, MARS. J.A. McLaughlin1 and A.K. Davatzes2, 1Temple University, [email protected], 2Temple University, [email protected]. Introduction: Crater erosion and morphology are Level of Degradation (LOD) was defined for each indicators of the climatic and erosional history of the crater using depth to diameter ratios (d/D) and percent- area in which the crater is found [1][2]. Here we pre- age of crater rim remaining. This categorizes craters sent a detailed analysis of crater erosion and morphol- into four types; 1 is the least degraded and 4 is the ogy in the Isidis Planitia Basin region. The goal of this most degraded. Criteria are based on the following: work is to produce a thorough database of crater prop- erties and document the modification processes that dominate locally and regionally. Crater degradation, age, and geomorphology are all considered and cross- correlated to narrow down the timing and dominance of persistent fluvial, lacustrine, and volcanic processes Floor features are complex and variable, but struc- on Mars. These geologic processes modify the crater tures indicative of the following processes were identi- rims and floor, often in distinguishable ways that pro- fied: Volcanic, Aeolian, Impact, Glacial, Mass Wast- vide insight into past environmental conditions. These ing, and Water Interaction. When possible, percent environments may hold clues to past habitable envi- floor cover of features such as lava flows, mass wast- ronments that are of particular interest for future mis- ing, dune and dust coverage were documented. -
1 Cross-Calibration of Laser-Induced Breakdown Spectroscopy (LIBS)
ISSI/ISSI-BJ Joint Call for Proposals 2018 International Teams in Space and Earth Sciences Cross-calibration of Laser-Induced Breakdown Spectroscopy (LIBS) instruments for planetary exploration. 1 Summary of the project : A revolutionary technique for planetary science: Laser-induced Breakdown Spectroscopy (LIBS) is an active analytical technique that makes use of a pulsed laser to ablate material of interest at a distance. The atoms in the high temperature plasma emit at specific wavelengths from the UV to near- IR and the light can be analyzed by spectrometry to determine the composition of the target [1]. Since 2012, LIBS has been successfully used under low atmospheric pressure for exploring the geology of Mars at Gale Crater with the Mars Science Laboratory rover’s ChemCam instrument [2-4]. LIBS can be used to analyze single regolith mineral particles and larger rocks, giving major and minor elements compositions. Moreover, LIBS is sensitive to volatile elements (H, Na, etc.) that are of intrinsic interest to understand key planetary processes. The generated shock wave can also ablate dust covering rocks to allow further analysis by other instruments on the mission platform (rover, lander). In order to quantify the elemental composition of various targets, large laboratory samples analyses are required for calibration, with ChemCam’s calibration database containing more than 400 standards [5-6]. LIBS is becoming international: Due to its ease of deployment and rapidity of analysis, LIBS has shown a great potential as a chemistry survey instrument for the next generation of in situ space missions to planets, satellites and small bodies. In the next couple of years, three more LIBS space instruments will be sent for planetary exploration by teams representing several different nationalities In 2018, the Indian space mission to the Moon Chandrayaan 2 will comprise a rover equipped with a small portable LIBS instrument for regolith reconnaissance around the landing site [7]. -
A Unified Plane Coordinate Reference System
This dissertation has been microfilmed exactly as received COLVOCORESSES, Alden Partridge, 1918- A UNIFIED PLANE COORDINATE REFERENCE SYSTEM. The Ohio State University, Ph.D., 1965 Geography University Microfilms, Inc., Ann Arbor, Michigan A UNIFIED PLANE COORDINATE REFERENCE SYSTEM DISSERTATION Presented in Partial Fulfillment of the Requirements for The Degree Doctor of Philosophy in the Graduate School of The Ohio State University Alden P. Colvocoresses, B.S., M.Sc. Lieutenant Colonel, Corps of Engineers United States Army * * * * * The Ohio State University 1965 Approved by Adviser Department of Geodetic Science PREFACE This dissertation was prepared while the author was pursuing graduate studies at The Ohio State University. Although attending school under order of the United States Army, the views and opinions expressed herein represent solely those of the writer. A list of individuals and agencies contributing to this paper is presented as Appendix B. The author is particularly indebted to two organizations, The Ohio State University and the Army Map Service. Without the combined facilities of these two organizations the preparation of this paper could not have been accomplished. Dr. Ivan Mueller of the Geodetic Science Department of The Ohio State University served as adviser and provided essential guidance and counsel. ii VITA September 23, 1918 Born - Humboldt, Arizona 1941 oo.oo.o BoS. in Mining Engineering, University of Arizona 1941-1945 .... Military Service, European Theatre 1946-1950 o . o Mining Engineer, Magma Copper -
Exploration of Mars by the European Space Agency 1
Exploration of Mars by the European Space Agency Alejandro Cardesín ESA Science Operations Mars Express, ExoMars 2016 IAC Winter School, November 20161 Credit: MEX/HRSC History of Missions to Mars Mars Exploration nowadays… 2000‐2010 2011 2013/14 2016 2018 2020 future … Mars Express MAVEN (ESA) TGO Future ESA (ESA- Studies… RUSSIA) Odyssey MRO Mars Phobos- Sample Grunt Return? (RUSSIA) MOM Schiaparelli ExoMars 2020 Phoenix (ESA-RUSSIA) Opportunity MSL Curiosity Mars Insight 2020 Spirit The data/information contained herein has been reviewed and approved for release by JPL Export Administration on the basis that this document contains no export‐controlled information. Mars Express 2003-2016 … First European Mission to orbit another Planet! First mission of the “Rosetta family” Up and running since 2003 Credit: MEX/HRSC First European Mission to orbit another Planet First European attempt to land on another Planet Original mission concept Credit: MEX/HRSC December 2003: Mars Express Lander Release and Orbit Insertion Collission trajectory Bye bye Beagle 2! Last picture Lander after release, release taken by VMC camera Insertion 19/12/2003 8:33 trajectory Credit: MEX/HRSC Beagle 2 was found in January 2015 ! Only 6km away from landing site OK Open petals indicate soft landing OK Antenna remained covered Lessons learned: comms at all time! Credit: MEX/HRSC Mars Express: so many missions at once Mars Mission Phobos Mission Relay Mission Credit: MEX/HRSC Mars Express science investigations Martian Moons: Phobos & Deimos: Ionosphere, surface, -
Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J. -
Mars Exploration - a Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani
Chapter Introductory Chapter: Mars Exploration - A Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani 1. Introduction Mars has been a goal of exploration programs of the most important space agencies all over the world for decades. It is, in fact, the most investigated celestial body of the Solar System. Mars robotic exploration began in the 1960s of the twentieth century by means of several space probes sent by the United States (US) and the Soviet Union (USSR). In the recent past, also European, Japanese, and Indian spacecrafts reached Mars; while other countries, such as China and the United Arab Emirates, aim to send spacecraft toward the red planet in the next future. 1.1 Exploration aims The high number of mission explorations to Mars clearly points out the impor- tance of Mars within the Solar System. Thus, the question is: “Why this great interest in Mars exploration?” The interest in Mars is due to several practical, scientific, and strategic reasons. In the practical sense, Mars is the most accessible planet in the Solar System [1]. It is the second closest planet to Earth, besides Venus, averaging about 360 million kilometers apart between the furthest and closest points in its orbit. Earth and Mars feature great similarities. For instance, both planets rotate on an axis with quite the same rotation velocity and tilt angle. The length of a day on Earth is 24 h, while slightly longer on Mars at 24 h and 37 min. The tilt of Earth axis is 23.5 deg, and Mars tilts slightly more at 25.2 deg [2].