Life on Mars (Lomars): a Bibliometric Study of Current Research and Future Perspectives
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Cosmic-Ray-Exposure Ages Martian Meteorites Million Years
Introduction to MMC 2012 someone keeps adding pieces as you go along (see my Introduction 2006). Most Martian meteorites are mafic As of the end of 2012, we now know of about 65 basalts. That is, they have an abundance of Fe and different meteorites from Mars with a total weight about Mg, are low in Si and Al and have a texture of 120 kilograms. Some fell as showers (e.g. Nakhla, intergrown minerals typical of terrestrial basalts (the Tissint), and some can be paired by common lithology, tradition has been to call them “shergottites”, after the age and fall location, but it is more instructive to first sample recognized as such). Some often have an consider how they are grouped by “launch pairs”. If abundance of large olivine crystals (so called olivine- you add the terrestrial age to the cosmic exposure age phyric). Others have an abundance of both high- and (CRE) you get the time when the meteorite was low-Ca pyroxene, with poikilitic textures and were launched off of Mars by impact. Since only rather large originally called “lherzolitic shergottites”. But it has impacts would do this, there must be a finite number now been recognized that there is a more fundamental of such impacts – hence grouping of samples. and better way to describe these rocks (Irving 2012). Now that we have such a large number of samples, it Figure 1 shows a crude summary of CRE that have is time to understand what we have and infer what we been determined for Martian meteorites. Note that can about Mars. -
Lafayette - 800 Grams Nakhlite
Lafayette - 800 grams Nakhlite Figure 1. Photograph showing fine ablation features Figure 2. Photograph of bottom surface of Lafayette of fusion crust on Lafayette meteorite. Sample is meteorite. Photograph from Field Museum Natural shaped like a truncated cone. This is a view of the top History, Chicago, number 62918. of the cone. Sample is 4-5 centimeters across. Photo- graph from Field Museum Natural History, Chicago, number 62913. Introduction According to Graham et al. (1985), “a mass of about 800 grams was noticed by Farrington in 1931 in the geological collections in Purdue University in Lafayette Indiana.” It was first described by Nininger (1935) and Mason (1962). Lafayette is very similar to the Nakhla and Governador Valadares meteorites, but apparently distinct from them (Berkley et al. 1980). Lafayette is a single stone with a fusion crust showing Figure 3. Side view of Lafayette. Photograph from well-developed flow features from ablation in the Field Museum Natural History, Chicago, number Earth’s atmosphere (figures 1,2,3). The specimen is 62917. shaped like a rounded cone with a blunt bottom end. It was apparently oriented during entry into the Earth’s that the water released during stepwise heating of atmosphere. Note that the fine ablation features seen Lafayette was enriched in deuterium. The alteration on Lafayette have not been reported on any of the assemblages in Lafayette continue to be an active field Nakhla specimens. of research, because it has been shown that the alteration in Lafayette occurred on Mars. Karlsson et al. (1992) found that Lafayette contained the most extra-terrestrial water of any Martian Lafayette is 1.32 b.y. -
Sequestration of Martian CO2 by Mineral Carbonation
ARTICLE Received 11 Jun 2013 | Accepted 24 Sep 2013 | Published 22 Oct 2013 DOI: 10.1038/ncomms3662 OPEN Sequestration of Martian CO2 by mineral carbonation Tim Tomkinson1, Martin R. Lee2, Darren F. Mark1 & Caroline L. Smith3,4,5 Carbonation is the water-mediated replacement of silicate minerals, such as olivine, by carbonate, and is commonplace in the Earth’s crust. This reaction can remove significant quantities of CO2 from the atmosphere and store it over geological timescales. Here we present the first direct evidence for CO2 sequestration and storage on Mars by mineral carbonation. Electron beam imaging and analysis show that olivine and a plagioclase feldspar- rich mesostasis in the Lafayette meteorite have been replaced by carbonate. The susceptibility of olivine to replacement was enhanced by the presence of smectite veins along which CO2-rich fluids gained access to grain interiors. Lafayette was partially carbonated during the Amazonian, when liquid water was available intermittently and atmospheric CO2 concentrations were close to their present-day values. Earlier in Mars’ history, when the planet had a much thicker atmosphere and an active hydrosphere, carbonation is likely to have been an effective mechanism for sequestration of CO2. 1 Scottish Universities Environmental Research Centre, Rankine Avenue, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK. 2 School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow G12 8QQ, UK. 3 Department of Earth Sciences, Natural History Museum, Cromwell Road, London SW7 5BD, UK. 4 ESA ESTEC, Keplerlaan 1, 200 AG Noordwijk, The Netherlands. 5 UK Space Agency, Atlas Building, Harwell Oxford, Didcot, Oxfordshire OX11 0QX, UK. -
Secondary Minerals in the Nakhlite Meteorite Yamato 000593: Distinguishing Martian from Terrestrial Alteration Products
46th Lunar and Planetary Science Conference (2015) 2010.pdf SECONDARY MINERALS IN THE NAKHLITE METEORITE YAMATO 000593: DISTINGUISHING MARTIAN FROM TERRESTRIAL ALTERATION PRODUCTS. H. Breton1, M. R. Lee1, and D. F. Mark2 1School of Geographical and Earth Sciences, University of Glasgow, University Ave, Glasgow, Lanarkshire G12 8QQ, UK ([email protected]), 2Scottish Universities Environmental Research Center, Rankine Ave, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK Introduction: The nakhlites are olivine-bearing Methods: A thin section of Y-000593 was studied clinopyroxenites that formed in a Martian lava flow or using a Carl Zeiss Sigma field-emission SEM equipped shallow intrusion 1.3 Ga ago [1, 2]. They are scientifi- with an Oxford Instruments Aztec microanalysis sys- cally extremely valuable because they interacted with tem at the University of Glasgow. Chemical and miner- water-bearing fluids on Mars [3]. Fluid-rock interac- alogical identification within the secondary minerals tions led to the precipitation of secondary minerals, were obtained through backscattered electron (BSE) many of which are hydrous. The secondary minerals imaging and energy dispersive spectroscopy (EDS) consist in a mixture of poorly crystalline smectitic ma- mapping and quantitative microanalysis. terial and Fe-oxide, collectively called “iddingsite”, but Results and discussions: Y-000593 is an unbrec- also carbonate and sulphate [4]. The proportion, chem- ciated cumulate rock whose mineralogy is similar to istry and habit of the secondary minerals vary between other nakhlites: a predominance of augite and minor members of the Nakhlite group, which is thought to olivine phenocrysts surrounded by a microcrystalline reflect compositional variation of the fluid within the mesostasis [9]. -
Physical Properties of Martian Meteorites: Porosity and Density Measurements
Meteoritics & Planetary Science 42, Nr 12, 2043–2054 (2007) Abstract available online at http://meteoritics.org Physical properties of Martian meteorites: Porosity and density measurements Ian M. COULSON1, 2*, Martin BEECH3, and Wenshuang NIE3 1Solid Earth Studies Laboratory (SESL), Department of Geology, University of Regina, Regina, Saskatchewan S4S 0A2, Canada 2Institut für Geowissenschaften, Universität Tübingen, 72074 Tübingen, Germany 3Campion College, University of Regina, Regina, Saskatchewan S4S 0A2, Canada *Corresponding author. E-mail: [email protected] (Received 11 September 2006; revision accepted 06 June 2007) Abstract–Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet’s surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability. -
The Physical Properties of Asteroids
University of Central Florida STARS Electronic Theses and Dissertations, 2020- 2020 The Physical Properties of Asteroids Leos Pohl University of Central Florida Part of the Physics Commons Find similar works at: https://stars.library.ucf.edu/etd2020 University of Central Florida Libraries http://library.ucf.edu This Doctoral Dissertation (Open Access) is brought to you for free and open access by STARS. It has been accepted for inclusion in Electronic Theses and Dissertations, 2020- by an authorized administrator of STARS. For more information, please contact [email protected]. STARS Citation Pohl, Leos, "The Physical Properties of Asteroids" (2020). Electronic Theses and Dissertations, 2020-. 269. https://stars.library.ucf.edu/etd2020/269 THE PHYSICAL PROPERTIES OF ASTEROIDS by LEOS POHL B.S. Charles University, Prague, 2011 M.S. Charles University, Prague, 2014 A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics in the Department of Physics in the College of Sciences at the University of Central Florida Orlando, Florida Summer Term 2020 Major Professor: Daniel T. Britt © 2020 LEOS POHL ii ABSTRACT The Small Bodies of the Solar System are leftover material from the formation of planets. Compared with planetary bodies, they have undergone relatively little transfor- mation. Embedded in their physical properties, are clues to the conditions and processes that took place since the condensation of the Solar Nebula. Furthermore, asteroids are sources of raw materials that have become a topic of significant interest. In this dis- sertation, I explore several properties of asteroid material: strength of asteroids, their shielding properties against high energetic particles and their water content. -
Fine-Grained Antarctic Micrometeorites and Weathered Carbonaceous Chondrites As Possible Analogues of Ceres Surface: Implications on Its Evolution
EPSC Abstracts Vol. 12, EPSC2018-1024, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Fine-grained Antarctic micrometeorites and weathered carbonaceous chondrites as possible analogues of Ceres surface: implications on its evolution. Jacopo Nava (1), Cristian Carli (2), Ernesto Palomba (2), Alessandro Maturilli (3) and Matteo Massironi (1) (1) Università degli studi di Padova – Dipartimento di Geoscienze, Padova, Italy ([email protected]) (2) IAPS-INAF, Istituto Nazionale di Astrofisica e Planetologia Spaziali, Roma, Italy (3) Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany. Abstract more weathered and are mainly made of jarosite plus Fe-carbonates and Fe-K sulfides. All of these IR spectra of several micrometeorites (MMs) and samples show the constant presence of carbon Antarctic weathered carbonaceous chondrites compound, which can be poorly graphitized C. (AWCCs) have been acquired and compared to Ceres Phyllosilicates are rare. For what concerns the spectra. We propose these samples as possible AWCCs we found the CM2 sample GRA 98005 with analogues of Ceres. This allowed us to define a more weathering grade Ce that had one side exposed to the precise composition of Ceres and to suggest a Antarctic environment, and is thus heavily altered, possible evolution of this body. and one side that has been preserved with a pristine composition. Spectra on the pristine side are flat and almost featureless. On the contrary spectra of the 1. Introduction weathered side tend to have a shape close to the average Ceres spectra. This meteorite, on the Ceres is an icy body with a surface composition close weathered side, is dominated by Fe-oxides, Ca-Fe to the carbonaceous chondrites (CCs) [1] that carbonates, anidrite and gypsum plus enstatite and suffered aqueous alteration [2] and geothermal forsterite. -
Aqueous Alteration in Martian Meteorites: Comparing Mineral Relations in Igneous-Rock Weathering of Martian Meteorites and in the Sedimentary Cycle of Mars
AQUEOUS ALTERATION IN MARTIAN METEORITES: COMPARING MINERAL RELATIONS IN IGNEOUS-ROCK WEATHERING OF MARTIAN METEORITES AND IN THE SEDIMENTARY CYCLE OF MARS MICHAEL A. VELBEL Department of Geological Sciences, 206 Natural Science Building, Michigan State University, East Lansing, Michigan 48824-1115 USA e-mail: [email protected] ABSTRACT: Many of the minerals observed or inferred to occur in the sediments and sedimentary rocks of Mars, from a variety of Mars-mission spacecraft data, also occur in Martian meteorites. Even Martian meteorites recovered after some exposure to terrestrial weathering can preserve preterrestrial evaporite minerals and useful information about aqueous alteration on Mars, but the textures and textural contexts of such minerals must be examined carefully to distinguish preterrestrial evaporite minerals from occurrences of similar minerals redistributed or formed by terrestrial processes. Textural analysis using terrestrial microscopy provides strong and compelling evidence for preterrestrial aqueous alteration products in a numberof Martian meteorites. Occurrences of corroded primary rock-forming minerals and alteration products in meteorites from Mars cover a range of ages of mineral–water interaction, from ca. 3.9 Ga (approximately mid-Noachian), through one or more episodes after ca. 1.3 Ga (approximately mid–late Amazonian), through the last half billion years (late Amazonian alteration in young shergottites), to quite recent. These occurrences record broadly similar aqueous corrosion processes and formation of soluble weathering products over a broad range of times in the paleoenvironmental history of the surface of Mars. Many of the same minerals (smectite-group clay minerals, Ca-sulfates, Mg-sulfates, and the K-Fe–sulfate jarosite) have been identified both in the Martian meteorites and from remote sensing of the Martian surface. -
SCIENCE CITATION INDEX EXPANDED - JOURNAL LIST Total Journals: 8631
SCIENCE CITATION INDEX EXPANDED - JOURNAL LIST Total journals: 8631 1. 4OR-A QUARTERLY JOURNAL OF OPERATIONS RESEARCH 2. AAPG BULLETIN 3. AAPS JOURNAL 4. AAPS PHARMSCITECH 5. AATCC REVIEW 6. ABDOMINAL IMAGING 7. ABHANDLUNGEN AUS DEM MATHEMATISCHEN SEMINAR DER UNIVERSITAT HAMBURG 8. ABSTRACT AND APPLIED ANALYSIS 9. ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY 10. ACADEMIC EMERGENCY MEDICINE 11. ACADEMIC MEDICINE 12. ACADEMIC PEDIATRICS 13. ACADEMIC RADIOLOGY 14. ACCOUNTABILITY IN RESEARCH-POLICIES AND QUALITY ASSURANCE 15. ACCOUNTS OF CHEMICAL RESEARCH 16. ACCREDITATION AND QUALITY ASSURANCE 17. ACI MATERIALS JOURNAL 18. ACI STRUCTURAL JOURNAL 19. ACM COMPUTING SURVEYS 20. ACM JOURNAL ON EMERGING TECHNOLOGIES IN COMPUTING SYSTEMS 21. ACM SIGCOMM COMPUTER COMMUNICATION REVIEW 22. ACM SIGPLAN NOTICES 23. ACM TRANSACTIONS ON ALGORITHMS 24. ACM TRANSACTIONS ON APPLIED PERCEPTION 25. ACM TRANSACTIONS ON ARCHITECTURE AND CODE OPTIMIZATION 26. ACM TRANSACTIONS ON AUTONOMOUS AND ADAPTIVE SYSTEMS 27. ACM TRANSACTIONS ON COMPUTATIONAL LOGIC 28. ACM TRANSACTIONS ON COMPUTER SYSTEMS 29. ACM TRANSACTIONS ON COMPUTER-HUMAN INTERACTION 30. ACM TRANSACTIONS ON DATABASE SYSTEMS 31. ACM TRANSACTIONS ON DESIGN AUTOMATION OF ELECTRONIC SYSTEMS 32. ACM TRANSACTIONS ON EMBEDDED COMPUTING SYSTEMS 33. ACM TRANSACTIONS ON GRAPHICS 34. ACM TRANSACTIONS ON INFORMATION AND SYSTEM SECURITY 35. ACM TRANSACTIONS ON INFORMATION SYSTEMS 36. ACM TRANSACTIONS ON INTELLIGENT SYSTEMS AND TECHNOLOGY 37. ACM TRANSACTIONS ON INTERNET TECHNOLOGY 38. ACM TRANSACTIONS ON KNOWLEDGE DISCOVERY FROM DATA 39. ACM TRANSACTIONS ON MATHEMATICAL SOFTWARE 40. ACM TRANSACTIONS ON MODELING AND COMPUTER SIMULATION 41. ACM TRANSACTIONS ON MULTIMEDIA COMPUTING COMMUNICATIONS AND APPLICATIONS 42. ACM TRANSACTIONS ON PROGRAMMING LANGUAGES AND SYSTEMS 43. ACM TRANSACTIONS ON RECONFIGURABLE TECHNOLOGY AND SYSTEMS 44. -
The Nakhlite Meteorites: Augite-Rich Igneous Rocks from Mars ARTICLE
ARTICLE IN PRESS Chemie der Erde 65 (2005) 203–270 www.elsevier.de/chemer INVITED REVIEW The nakhlite meteorites: Augite-rich igneous rocks from Mars Allan H. Treiman Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058-1113, USA Received 22 October 2004; accepted 18 January 2005 Abstract The seven nakhlite meteorites are augite-rich igneous rocks that formed in flows or shallow intrusions of basaltic magma on Mars. They consist of euhedral to subhedral crystals of augite and olivine (to 1 cm long) in fine-grained mesostases. The augite crystals have homogeneous cores of Mg0 ¼ 63% and rims that are normally zoned to iron enrichment. The core–rim zoning is cut by iron-enriched zones along fractures and is replaced locally by ferroan low-Ca pyroxene. The core compositions of the olivines vary inversely with the steepness of their rim zoning – sharp rim zoning goes with the most magnesian cores (Mg0 ¼ 42%), homogeneous olivines are the most ferroan. The olivine and augite crystals contain multiphase inclusions representing trapped magma. Among the olivine and augite crystals is mesostasis, composed principally of plagioclase and/or glass, with euhedra of titanomagnetite and many minor minerals. Olivine and mesostasis glass are partially replaced by veinlets and patches of iddingsite, a mixture of smectite clays, iron oxy-hydroxides and carbonate minerals. In the mesostasis are rare patches of a salt alteration assemblage: halite, siderite, and anhydrite/ gypsum. The nakhlites are little shocked, but have been affected chemically and biologically by their residence on Earth. Differences among the chemical compositions of the nakhlites can be ascribed mostly to different proportions of augite, olivine, and mesostasis. -
Trajectory Optimization for First Human Asteroid Exploration Mission
Journal of Aircraft and Spacecraft Technology Original Research Paper Trajectory Optimization for First Human Asteroid Exploration Mission 1Atiksha Sharma and 2Santosh Kosambe 1Independent Researcher, Nagpur, India 2Independent Researcher, Pune, India Article history Abstract: After the successful completion of robotic expeditions on Mars, Received: 06-03-2020 an ultimate goal was set for space fairing nations and agencies around the Revised: 21-04-2020 world to send astronauts to Mars by 2030. Unfortunately, a mission to Mars Accepted: 27-07-2020 would last upwards for years meanwhile several asteroids fly close to the Earth. A manned trip to an asteroid would be a valuable stepping stone Corresponding Author: Atiksha Sharma towards a manned mission to Mars, as the mission time can be reduced to a Independent Researcher, few months round-trip. In addition to gaining experience with manned Nagpur, India travel through deep space, a mission to an asteroid would provide Email: [email protected] experience overcoming a unique challenge of rendezvousing with a foreign object in microgravity. Since most of the known asteroids that are close enough to Earth to be viable targets are less than 300 m in diameter, chances are the selected asteroid will not have a significant gravitational field. Near Earth Asteroids (NEAs) have orbits that bring them into close proximity with Earth’s orbit making them both a unique hazard to life on Earth and a unique opportunity for science and exploration. A specific case study was therefore undertaken to shortlist such NEAs that are accessible for round-trip human missions using heavy lift launch architecture. -
Bio-Inspired Method for Close-Proximity Operations on a Near- Earth Asteroid
University of Texas at El Paso ScholarWorks@UTEP Open Access Theses & Dissertations 2020-01-01 Bio-Inspired Method for Close-Proximity Operations on a Near- Earth Asteroid Rene Alberto Valenzuela Najera University of Texas at El Paso Follow this and additional works at: https://scholarworks.utep.edu/open_etd Part of the Aerospace Engineering Commons Recommended Citation Valenzuela Najera, Rene Alberto, "Bio-Inspired Method for Close-Proximity Operations on a Near-Earth Asteroid" (2020). Open Access Theses & Dissertations. 3053. https://scholarworks.utep.edu/open_etd/3053 This is brought to you for free and open access by ScholarWorks@UTEP. It has been accepted for inclusion in Open Access Theses & Dissertations by an authorized administrator of ScholarWorks@UTEP. For more information, please contact [email protected]. BIO-INSPIRED METHOD FOR CLOSE-PROXIMITY OPERATIONS ON A NEAR-EARTH ASTEROID RENÉ ALBERTO VALENZUELA NÁJERA Doctoral Program in Mechanical Engineering APPROVED: Angel Flores Abad, Ph.D., Chair Louis Everett, Ph.D. Co-Chair Jack F. Chessa, Ph. D Virgilio Gonzalez, Ph.D. Stephen L. Crites, Jr., Ph.D. Dean of the Graduate School Copyright © by René Alberto Valenzuela Nájera 2020 Dedication This work is dedicated to all the people who dedicate time to teach me, people have been by my side to support me in difficult times, for all my family and especially my Father and Mother who have always been present in my successes and failures. BIO-INSPIRED METHOD FOR CLOSE-PROXIMITY OPERATIONS ON A NEAR-EARTH ASTEROID by RENÉ ALBERTO VALENZUELA