DOCSLIB.ORG

Curie Temperature of Weakly Shocked Target Basalts at the Lonar Impact Crater, India A

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Curie Temperature of Weakly Shocked Target Basalts at the Lonar Impact Crater, India A Agarwal and Alva‑Valdivia Earth, Planets and Space (2019) 71:141 https://doi.org/10.1186/s40623‑019‑1120‑9 EXPRESS LETTER Open Access Curie temperature of weakly shocked target basalts at the Lonar impact crater, India A. Agarwal1* and L. M. Alva‑Valdivia2 Abstract The study investigates Curie temperature (TC), bulk magnetic susceptibility, hysteresis, and X‑ray difraction pattern of in situ target basalts of Lonar impact crater, India. The main magnetic phase in the target basalt is low‑Ti titanomag‑ netite. This study reveals an increase in TC and decrease in magnetic susceptibility and in full width at half maxima of the 311 peaks of titanomagnetite with distance from the crater center. Changes in crystal lattice of titanomagnetite, such as straining of 311 peaks, decrease in apparent crystallite size, and grain fragmentation may be among the pos‑ sible reasons for the observed trends in TC and magnetic susceptibility. However, they both do not show any correla‑ tion between each other, indicating that diferent shock‑induced processes afect them. Keywords: Lonar impact crater, Variation in Curie temperature, Variation in bulk magnetic susceptibility, X‑ray difraction pattern Introduction 1941; Iizumi et al. 1982). At temperatures between TV Magnetite is a common ferrimagnetic mineral in the ter- and Curie temperature—TC (~ 856 K or 582.85 °C), it is restrial and extraterrestrial rocks. Magnetite and other cubic, and it is ferrimagnetic due to an anti-ferromag- ferromagnetic minerals are a source of magnetic anoma- netic coupling of Fe(III) in tetrahedral and octahedral lies associated with terrestrial and extraterrestrial impact sites and Fe(II) in octahedral sites (Néel 1948; Tarling and craters and, therefore, play an important role in their dis- Hrouda 1993). Beyond TC, it is paramagnetic (Shull et al. covery and mapping (e.g., Pilkington and Grieve 1992; 1951), due to the loss of magnetic ordering (Harrison and Plado et al. 1999; Gilder et al. 2018). Moreover, behavior Putnis 1995, 1996). of magnetite and other ferromagnetic minerals at various Titanomagnetites form a solid-solution series shock pressures has been used to identify the magnetic (Fe3-xTixO4) with magnetite (0 = x) and ulvöspinel (x = 1) mineralogy of Mars (Louzada et al. 2011). Although criti- as the two end members. Te dependence of magnetite cal for impact cratering research on Earth and elsewhere, TC upon the chemical composition is well established. the behavior of magnetite, in weakly shocked rocks, is Tere is a negative correlation between TC and the not well understood. ulvöspinel content, ‘x’ (e.g., Akimoto et al. 1957; Özdemir Magnetite has a typical inverse spinel structure with and O’Reilly 1981; Moskowitz et al. 1998; Lattard et al. Fe(II) and Fe(III) disordered in the octahedral sites and 2006). Tis correlation is owed to the change in lattice fully occupied tetrahedrons by Fe(III) cation (Verwey parameters due to replacement of Fe cation by Ti (Aki- and Haayman 1941). At temperatures below Verwey moto et al. 1957). transition (TV), about 110–120 K, magnetite has an Another factor afecting TC is hydrostatic pressure. orthorhombic crystal structure (Verwey and Haayman TC of titanomagnetite, with ulvöspinel component from 0 to 0.7, increases linearly with static pressures up to 6 GPa (Samara and Giardini 1969; Schult 1970). Under *Correspondence: amar@daad‑alumni.de 1 Albert‑Ludwigs‑Universität Freiburg, Institut für Geo‑ und hydrostatic pressure, a cubic crystal, such as that of Umweltnaturwissenschaften, Albertstraße 23b, 79104 Freiburg, Germany magnetite, results in a cubic unit cell with decreased Full list of author information is available at the end of the article interionic distances (barring any phase transformation). © The Author(s) 2019. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creat iveco mmons .org/licen ses/by/4.0/. Agarwal and Alva‑Valdivia Earth, Planets and Space (2019) 71:141 Page 2 of 8 Tis causes increased interionic exchange and higher knowledge, this is the frst report of such correlation TC (Samara and Giardini 1969). However, a similar from weakly shocked rocks of a natural crater. direct correlation between crystallographic changes Geological setting and rock magnetic properties and TC due to dynamic shock pressure is not yet estab- lished. Tis may be partly owed to lack of sufcient Lonar crater (19° 58′ N, 76° 31′ E) in the Buldana district experimental investigations and partly due to com- of India is a hypervelocity impact crater excavated in the plex shock wave behavior (refection and refraction) ca. 65 Ma tholeiitic Deccan basalt (Hagerty and Newsom due to heterogeneity in rocks at natural craters. Shock 2003; Maloof et al. 2010). Some studies using fssion waves from natural and experimental craters may indi- track and thermoluminescence dating suggested that the rectly afect TC by fracturing the magnetic grains, thus Lonar impact occurred 50 ka (Fredriksson et al. 1973), facilitating hydrothermal alteration to increase the while other reports using 40Ar/39Ar dating argue that the proportion of non-stoichiometric magnetite (Kontny impact crater is ca. 570 ka in age (Jourdan et al. 2011). et al. 2018). Te grain fragmentation may also trans- Te ~ 1.88 km wide simple crater is 150 m deep from form multi-domain magnetite (MD) to pseudo-single the rim and is flled with a 7–10-m-deep lake. Te lake domain (PSD) or single domain (SD), thus reducing the is flled with 30–100-m-thick unconsolidated postim- magnetic susceptibility (e.g., Reznik et al. 2016). pact sediments, which are underlain by ~ 225 m of impact Tis study investigates the variation in TC, magnetic breccia (Fredriksson et al. 1973; Fudali et al. 1980; Grieve susceptibility, and XRD pattern in the weakly shocked et al. 1989). Te Lonar crater is an excellent analog of target basalts (< 3 GPa) of Lonar impact structure. Te extraterrestrial impact craters on basalt. It is relatively results show a systematic change in these properties pristine and has not undergone any postimpact tecto- with distance from the center of Lonar impact cra- nism (Maloof et al. 2010; Agarwal et al. 2016). ter, i.e., with a change in peak shock pressure. To our Te target basalt is comprised of fve very similar and homogenous Deccan basalt fows (Fig. 1), whose Fig. 1 Map of Lonar crater (after Maloof et al. 2010) with sampling sites of this study. Lava fows: Tf0, Tf1, Tf2, Tf3, Tf4, Tf5, and Tf6. Coordinates are represented in UTM—WGS84 Agarwal and Alva‑Valdivia Earth, Planets and Space (2019) 71:141 Page 3 of 8 geochemical, textural, and rock magnetic properties have magnetic susceptibility of each sample was measured at been studied in detail (e.g., Kiefer et al. 1976; Hagerty room temperature in the Kappabridge (KLY-4S). and Newsom 2003). Te TiO2 content of diferent fows Hysteresis curves were determined using Alternating of the target basalt is similar (Osae et al. 2005). Each fow Gradient Field Magnetometer Micromag apparatus in is ~ 8 to 40 m thick, separated by horizons of red and felds up to 1.4 T. Te curves allow calculating the rema- green paleosols and has vesicles flled with secondary nence of coercivity-to-coercive force (Hcr/Hc) and the materials like chlorite, zeolite, quartz, and brown limo- remanent magnetization-to-saturation remanence (Mrs/ nite, and most have a chill margin at their bottom and Ms) ratios of each sample. Tese ratios are used to esti- a heated and brecciated top (Ghosh and Bhaduri 2003). mate the relative proportions of the single domain (SD), Te fows exposed in the Lonar crater wall are chemi- multi-domain (MD), and pseudo-single domain (PSD) cally similar and are classifed as relatively low-K tholei- grains (Dunlop 2002a, b). In general, the ratio of Mrs/ itic intra-plate basalts, with minor Fe and Ca enrichment Ms is higher for more SD materials and lower for more and slight Mg and Al depletion compared to “average” MD-like materials. Agarwal et al. (2016) applied stepwise tholeiites (Osae et al. 2005). All of the shocked basalts increasing uniaxial feld on the samples to calculate the are altered, containing vesicles and veins full of carbonate saturated and non-saturated isothermal remanent mag- and clays (Hagerty and Newsom 2003). netization (IRM) acquisition curves. Tese curves were Te alteration is recorded as young (< 50 kya) viscous used to determine the median destructive feld (MDF). and/or chemical remanent magnetization in the tar- Te samples were then divided into magnetically hard, get rocks (Louzada et al. 2008; Arif et al. 2012; Agarwal soft, and intermediate groups, based on the dominant et al. 2016). Te target basalts also present an older com- magnetic domain state and the MDF. ponent similar to the Deccan direction (Louzada et al. Te XRD pattern of magnetically hard basalts (domi- 2008; Agarwal et al. 2016). Te main magnetic phase in nated by SD) was measured with a Siemens D500 difrac- the target basalt is low-Ti titanomagnetite with a mag- tometer using a Cu-Ka anode.
Load more

Recommended publications
  • Martian Crater Morphology
    ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter.
    [Show full text]
  • Warfare in a Fragile World: Military Impact on the Human Environment
    Recent Slprt•• books World Armaments and Disarmament: SIPRI Yearbook 1979 World Armaments and Disarmament: SIPRI Yearbooks 1968-1979, Cumulative Index Nuclear Energy and Nuclear Weapon Proliferation Other related •• 8lprt books Ecological Consequences of the Second Ihdochina War Weapons of Mass Destruction and the Environment Publish~d on behalf of SIPRI by Taylor & Francis Ltd 10-14 Macklin Street London WC2B 5NF Distributed in the USA by Crane, Russak & Company Inc 3 East 44th Street New York NY 10017 USA and in Scandinavia by Almqvist & WikseH International PO Box 62 S-101 20 Stockholm Sweden For a complete list of SIPRI publications write to SIPRI Sveavagen 166 , S-113 46 Stockholm Sweden Stoekholol International Peace Research Institute Warfare in a Fragile World Military Impact onthe Human Environment Stockholm International Peace Research Institute SIPRI is an independent institute for research into problems of peace and conflict, especially those of disarmament and arms regulation. It was established in 1966 to commemorate Sweden's 150 years of unbroken peace. The Institute is financed by the Swedish Parliament. The staff, the Governing Board and the Scientific Council are international. As a consultative body, the Scientific Council is not responsible for the views expressed in the publications of the Institute. Governing Board Dr Rolf Bjornerstedt, Chairman (Sweden) Professor Robert Neild, Vice-Chairman (United Kingdom) Mr Tim Greve (Norway) Academician Ivan M£ilek (Czechoslovakia) Professor Leo Mates (Yugoslavia) Professor
    [Show full text]
  • New Chryse and the Provinces
    New Chryse and the Provinces The city of New Chryse is actually several connected cities. The Upper City is located on a break in the crater rim, looking down past a steep rock to the Lower City. Inside the da Vinci crater rim lies the Inner City, also known as the Old City – Red Era tunnels and cave shelters, as well as several nanocomposite towers and cupolas on Mona Lys Ridge looking down on the lower parts of the city. The Lower city lies in a valley sloping down to the Harbour City, which fills a crater 20 kilometres to the East. The Harbour City crater is connected to Camiling Bay and the sea through two canyons and is very well protected from both wind and ice. South of the Lower City and Harbour City lies The Slopes, a straight slope into the sea that is covered with sprawl and slums. Mona Lys Ridge is a mixture of palatial estates surrounded by gardens, imposing official imperial buildings and towering ancient structures used by the highest ranks of the Empire. The central imperial administration and especially the Council is housed in the Deimos Needle, a diamondoid tower that together with its sibling the Phobos Needle dominate the skyline. Escalators allow swift and discreet transport down to the lower levels of the city, and can easily be defended by the police force. North of Mona Lys lies a secluded garden city for higher administrators, guild officials and lesser nobility. The Inner City is to a large extent part of Mona Lys, although most of the inhabitants of Mona Lys do not care much for the dusty old tunnels and hidden vaults – that is left to the Guild of Antiquarians who maintain and protect it.
    [Show full text]
  • Magnetized Impact Craters
    Icarus xxx (2011) xxx–xxx Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Predicted and observed magnetic signatures of martian (de)magnetized impact craters ⇑ Benoit Langlais a, , Erwan Thébault b a CNRS UMR 6112, Université de Nantes, Laboratoire de Planétologie et Géodynamique, 2 Rue de la Houssinière, F-44000 Nantes, France b CNRS UMR 7154, Institut de Physique du Globe de Paris, Équipe de Géomagnétisme, 1 Rue Cuvier, F-75005 Paris, France article info abstract Article history: The current morphology of the martian lithospheric magnetic field results from magnetization and Received 3 May 2010 demagnetization processes, both of which shaped the planet. The largest martian impact craters, Hellas, Revised 6 January 2011 Argyre, Isidis and Utopia, are not associated with intense magnetic fields at spacecraft altitude. This is Accepted 6 January 2011 usually interpreted as locally non- or de-magnetized areas, as large impactors may have reset the mag- Available online xxxx netization of the pre-impact material. We study the effects of impacts on the magnetic field. First, a care- ful analysis is performed to compute the impact demagnetization effects. We assume that the pre-impact Keywords: lithosphere acquired its magnetization while cooling in the presence of a global, centered and mainly Mars, Surface dipolar magnetic field, and that the subsequent demagnetization is restricted to the excavation area cre- Mars, Interior Impact processes ated by large craters, between 50- and 500-km diameter. Depth-to-diameter ratio of the transient craters Magnetic fields is set to 0.1, consistent with observed telluric bodies. Associated magnetic field is computed between 100- and 500-km altitude.
    [Show full text]
  • Possible Origin of Chlorobenzene Detected by SAM Instrument at Gale Crater, Mars: Synergy of Iron Oxides and Perchlorate and Consequences for Organic Matter Analysis
    Eighth International Conference on Mars (2014) 1201.pdf Possible origin of chlorobenzene detected by SAM instrument at Gale crater, Mars: synergy of iron oxides and perchlorate and consequences for organic matter analysis. P. Francois1, P. Coll1, C. Szopa2, T. Georgelin3, A. Buch4, C. Freissinet5,6, I. Belmahdi4, A. McAdam5, J. Eigenbrode5, D. Glavin5, S. Kashyap5, A. R. Navarro- Gonzalez7, P. Mahaffy5 and M. Cabane2. [email protected]. 1LISA, Univ. Paris-Est Créteil, Univ. Denis Diderot & CNRS 94010 Créteil, France 2LATMOS, Univ. Pierre et Marie Curie, Univ. Versailles Saint- Quentin & CNRS, 75005 Paris, France 3LRS, Univ. Pierre et Marie Curie, Ivry sur Seine, France 4LGPM, Ecole Centrale de Paris, 92295 Châtenay-Malabry 5NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 6NASA Postdoctoral Program Administered by Oak Ridge Associated Universities, Oak Ridge, Tennessee 37831, USA 7Universidad Nacional Autónoma de México, México, D.F. 04510, Mexico Introduction: The Sample Analysis at Mars rates [5]. Apart from an oxychlorine phase, CB sam- (SAM) instrument on the Curiosity rover is designed to ples also contain iron oxides (e.g. hematite, magnetite) determine the inventory of organic and inorganic vola- [6] which could oxidize organic compounds and cata- tiles thermally evolved from solid samples notably by lyze their decomposition leading to differences in the using a combination of evolved gas analysis (EGA) amount and/or nature of the observed pyrolysis prod- and pyrolysis gas chromatography mass spectrometry ucts [7, 8]. A synergy between oxychlorine phases and (pyr-GC-MS) [1]. Multiple portions from three solid iron oxides in the presence of a carbon source can samples have been analyzed by SAM : a scoop of ba- potentially lead to the formation of CBZ, without any saltic sand at Rocknest (RN) and two drilled samples of specific need for aromatic precursors.
    [Show full text]
  • The Structure and Mechanical Properties of Hemp Fibers-Reinforced Poly(-Caprolactone)
    applied sciences Article The Structure and Mechanical Properties of Hemp Fibers-Reinforced Poly("-Caprolactone) Composites Modified by Electron Beam Irradiation Rafał Malinowski 1,* , Aneta Raszkowska-Kaczor 1, Krzysztof Moraczewski 2 , Wojciech Głuszewski 3 , Volodymyr Krasinskyi 4 and Lauren Wedderburn 1 1 Łukasiewicz Research Network—Institute for Engineering of Polymer Materials and Dyes, 55 M. Skłodowska-Curie Street, 87-100 Toru´n,Poland; [email protected] (A.R.-K.); [email protected] (L.W.) 2 Institute of Materials Engineering, Kazimierz Wielki University, 30 Chodkiewicza Street, 85-064 Bydgoszcz, Poland; [email protected] 3 Institute of Nuclear Chemistry and Technology, 16 Dorodna Street, 03-195 Warsaw, Poland; [email protected] 4 Department of Chemical Technology of Plastics Processing, Lviv Polytechnic National University, 12 Stepan Bandera Street, 79-013 Lviv, Ukraine; [email protected] * Correspondence: [email protected]; Tel.: +48-53-060-0220 Abstract: The need for the development of new biodegradable materials and modification of the properties the current ones possess has essentially increased in recent years. The aim of this study Citation: Malinowski, R.; was the comparison of changes occurring in poly("-caprolactone) (PCL) due to its modification by Raszkowska-Kaczor, A.; high-energy electron beam derived from a linear electron accelerator, as well as the addition of natural Moraczewski, K.; Głuszewski, W.; fibers in the form of cut hemp fibers. Changes to the fibers structure in the obtained composites and Krasinskyi, V.; Wedderburn, L. The the geometrical surface structure of sample fractures with the use of scanning electron microscopy Structure and Mechanical Properties were investigated.
    [Show full text]
  • Appendix I Lunar and Martian Nomenclature
    APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei
    [Show full text]
  • GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
    Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins.
    [Show full text]
  • The Impact Origin and Evolution of Chryse Planitia on Mars Revealed by Buried Craters
    ARTICLE https://doi.org/10.1038/s41467-019-12162-0 OPEN The impact origin and evolution of Chryse Planitia on Mars revealed by buried craters Lu Pan 1, Cathy Quantin-Nataf1, Sylvain Breton1 & Chloé Michaut 1 Large impacts are one of the most important processes shaping a planet’s surface. On Mars, the early formation of the Martian crust and the lack of large impact basins (only four unambiguously identified: Hellas, Argyre, Utopia, and Isidis) indicates that a large part of ’ 1234567890():,; early records of Mars impact history is missing. Here we show, in Chryse Planitia, the scarcity of buried impact craters in a near-circular area could be explained by a pre-existing topographic depression with more intense resurfacing. Spatially correlated with positive Bouguer anomaly, this near-circular region with a diameter of ~1090 km likely originated from an impact. This proposed large impact basin must have been quickly relaxed or buried after its formation more than 4.0 billion years ago and heavily modified by subsequent resurfacing events. We anticipate our study to open a new window to unravelling the buried records of early Martian bombardment record. 1 Université de Lyon, Université Claude Bernard Lyon 1, ENS de Lyon, CNRS, UMR 5276 Laboratoire de Géologie de Lyon -Terre, Planètes, Environnement, 69622 Villeurbanne, France. Correspondence and requests for materials should be addressed to L.P. (email: [email protected]) NATURE COMMUNICATIONS | (2019) 10:4257 | https://doi.org/10.1038/s41467-019-12162-0 | www.nature.com/naturecommunications 1 ARTICLE NATURE COMMUNICATIONS | https://doi.org/10.1038/s41467-019-12162-0 arge basin-forming impacts significantly modified planetary could be the original Chryse impact basin, which subsequently surfaces and crusts, especially in the first billion years of underwent heavy degradation.
    [Show full text]
  • The Demon Haunted World
    THE DEMON- HAUNTED WORLD Science as a Candle in the Dark CARL SAGAN BALLANTINE BOOKS • NEW YORK Preface MY TEACHERS It was a blustery fall day in 1939. In the streets outside the apartment building, fallen leaves were swirling in little whirlwinds, each with a life of its own. It was good to be inside and warm and safe, with my mother preparing dinner in the next room. In our apartment there were no older kids who picked on you for no reason. Just the week be- fore, I had been in a fight—I can't remember, after all these years, who it was with; maybe it was Snoony Agata from the third floor— and, after a wild swing, I found I had put my fist through the plate glass window of Schechter's drug store. Mr. Schechter was solicitous: "It's all right, I'm insured," he said as he put some unbelievably painful antiseptic on my wrist. My mother took me to the doctor whose office was on the ground floor of our building. With a pair of tweezers, he pulled out a fragment of glass. Using needle and thread, he sewed two stitches. "Two stitches!" my father had repeated later that night. He knew about stitches, because he was a cutter in the garment industry; his job was to use a very scary power saw to cut out patterns—backs, say, or sleeves for ladies' coats and suits—from an enormous stack of cloth. Then the patterns were conveyed to endless rows of women sitting at sewing machines.
    [Show full text]
  • Ebook < Impact Craters on Mars # Download
    7QJ1F2HIVR # Impact craters on Mars « Doc Impact craters on Mars By - Reference Series Books LLC Mrz 2012, 2012. Taschenbuch. Book Condition: Neu. 254x192x10 mm. This item is printed on demand - Print on Demand Neuware - Source: Wikipedia. Pages: 50. Chapters: List of craters on Mars: A-L, List of craters on Mars: M-Z, Ross Crater, Hellas Planitia, Victoria, Endurance, Eberswalde, Eagle, Endeavour, Gusev, Mariner, Hale, Tooting, Zunil, Yuty, Miyamoto, Holden, Oudemans, Lyot, Becquerel, Aram Chaos, Nicholson, Columbus, Henry, Erebus, Schiaparelli, Jezero, Bonneville, Gale, Rampart crater, Ptolemaeus, Nereus, Zumba, Huygens, Moreux, Galle, Antoniadi, Vostok, Wislicenus, Penticton, Russell, Tikhonravov, Newton, Dinorwic, Airy-0, Mojave, Virrat, Vernal, Koga, Secchi, Pedestal crater, Beagle, List of catenae on Mars, Santa Maria, Denning, Caxias, Sripur, Llanesco, Tugaske, Heimdal, Nhill, Beer, Brashear Crater, Cassini, Mädler, Terby, Vishniac, Asimov, Emma Dean, Iazu, Lomonosov, Fram, Lowell, Ritchey, Dawes, Atlantis basin, Bouguer Crater, Hutton, Reuyl, Porter, Molesworth, Cerulli, Heinlein, Lockyer, Kepler, Kunowsky, Milankovic, Korolev, Canso, Herschel, Escalante, Proctor, Davies, Boeddicker, Flaugergues, Persbo, Crivitz, Saheki, Crommlin, Sibu, Bernard, Gold, Kinkora, Trouvelot, Orson Welles, Dromore, Philips, Tractus Catena, Lod, Bok, Stokes, Pickering, Eddie, Curie, Bonestell, Hartwig, Schaeberle, Bond, Pettit, Fesenkov, Púnsk, Dejnev, Maunder, Mohawk, Green, Tycho Brahe, Arandas, Pangboche, Arago, Semeykin, Pasteur, Rabe, Sagan, Thira, Gilbert, Arkhangelsky, Burroughs, Kaiser, Spallanzani, Galdakao, Baltisk, Bacolor, Timbuktu,... READ ONLINE [ 7.66 MB ] Reviews If you need to adding benefit, a must buy book. Better then never, though i am quite late in start reading this one. I discovered this publication from my i and dad advised this pdf to find out. -- Mrs. Glenda Rodriguez A brand new e-book with a new viewpoint.
    [Show full text]
  • Methane Release on Early Mars by Atmospheric Collapse and Atmospheric Reinflation
    Methane release on Early Mars by atmospheric collapse and atmospheric reinflation Edwin S. Kite1, Michael A. Mischna2, Peter Gao3,4, Yuk L. Yung2,5, Martin Turbet6,7,* 1. University of Chicago ([email protected]), Chicago, IL 60637. 2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109. 3. NASA Ames Research Center, Mountain View, CA 94035. 4. University of California, Berkeley, CA 94720. 5. California Institute of Technology, Pasadena, CA 91125. 6. Laboratoire de Météorologie Dynamique, IPSL, Sorbonne Universités, UPMC Univ Paris 06, CNRS, Paris 75005, France. 7. Observatoire Astronomique de l’Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland. * Currently Marie Sklodowska-Curie Fellow, Geneva Astronomical Observatory. Abstract. A candidate explanation for Early Mars rivers is atmospheric warming due to surface release of H2 or CH4 gas. However, it remains unknown how much gas could be released in a single event. We model the CH4 release by one mechanism for rapid release of CH4 from clathrate. By modeling how CH4-clathrate release is affected by changes in Mars’ obliquity and atmospheric composition, we find that a large fraction of total outgassing from CH4 clathrate occurs following Mars’ first prolonged atmospheric collapse. This atmosphere-collapse-initiated CH4-release mechanism has three stages. (1) Rapid collapse of Early Mars’ carbon dioxide atmosphere initiates a slower shift of water ice from high ground to the poles. (2) Upon subsequent CO2-atmosphere re-inflation and CO2-greenhouse warming, low-latitude clathrate decomposes and releases methane gas. (3) Methane can then perturb atmospheric chemistry and surface temperature, until photochemical processes destroy the methane.
    [Show full text]