A Model Explaining Some of the Catastrophic Effects of a Wave of Ice Bodies Passing Through the Solar System to Bring Water to Earth at the Time of Noah's Flood
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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. -
RSL), Described in the 5 August 2011 Science Report “Seasonal Flows on Warm Martian Slopes”
Animated GIFs to illustrate activity of Recurring Slope Lineae (RSL), described in the 5 August 2011 Science report “Seasonal Flows on Warm Martian Slopes”. All of these animated GIF files consist of a series of orthorectified HiRISE images over locations with RSL activity. Orthorectification corrects oblique images to show how the scene would appear from directly overhead. We perform this using HiRISE Digital Terrain Models (DTMs) at a scale of 1 m/posting. The orthorectified images are all at 0.25 m/pixel scale (or 0.5 m/pixel in cases noted below), so features smaller than 1-2 m diameter cannot be correctly rectified; the result is that small-scale features like boulders appear to wag back and forth. Each GIF is timed to dwell 2 seconds on the first and last frames and 1 second on intermediate frames, but network or computer performance may cause this to vary. The legend on each image gives the exact HiRISE image identifier; see http://uahirise.org/{image identified} for more information about each image. The legend also marks the year and seasonal identifier (Ls) for each image. The Mars years begin with the first years of Mars exploration by robot spacecraft. Ls stands for areocentric longitude of the sun, dividing the year into 360 degrees to mark the seasons. Ls = 180 is the beginning of southern spring, Ls = 270 is the beginning of southern summer, and Ls = 360 (or 0) is the beginning of southern autumn. Well-preserved crater on floor of Newton Crater Each of the gifs below are enhanced color sequences from different section of this crater slope, starting with faded RSL in MY29 (except one in which the color data was largely missing), then showing a sequence of RSL forming and fading in MY30. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Solar Wind Charge Exchange X-Ray Emission from Mars. Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V
Solar wind charge exchange X-ray emission from Mars. Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V. Kharchenko, Rosine Lallement To cite this version: Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V. Kharchenko, et al.. Solar wind charge exchange X-ray emission from Mars.: Model and data comparison. Astronomy and Astrophysics - A&A, EDP Sciences, 2012, 545, pp.A153. 10.1051/0004-6361/201219720. hal- 00731069 HAL Id: hal-00731069 https://hal.archives-ouvertes.fr/hal-00731069 Submitted on 2 Sep 2020 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. A&A 545, A153 (2012) Astronomy DOI: 10.1051/0004-6361/201219720 & c ESO 2012 Astrophysics Solar wind charge exchange X-ray emission from Mars Model and data comparison D. Koutroumpa1, R. Modolo1, G. Chanteur2, J.-Y., Chaufray1, V. Kharchenko3, and R. Lallement4 1 Université Versailles St-Quentin, CNRS/INSU, LATMOS-IPSL, 11 Bd d’Alembert, 78280 Guyancourt, France e-mail: [email protected] 2 Laboratoire de Physique des Plasmas, École Polytechnique, UPMC, CNRS, Palaiseau, France 3 Physics Department, University of Connecticut, Storrs, Connecticut, USA 4 GEPI, Observatoire de Paris, CNRS, 92195 Meudon, France Received 30 May 2012 / Accepted 17 August 2012 ABSTRACT Aims. -
The Prophecy That Is Shaping History
The Prophecy That Is Shaping History: New Research on Ezekiel’s Vision of the End Jon Mark Ruthven, PhD Ihab Griess, PhD Xulon Press 11350 Random Hills Drive #800 Fairfax, Virginia 22030 Copyright Jon Mark Ruthven © 2003 In memoriam Pamela Jessie Ruthven PhD, LCSW 26 March 1952 – 9 April 2001 Wife, mother, and faithful friend i Preface Great events in history often gather momentum and power long before they are recognized by the experts and commentators on world affairs. Easily one of the most neglected but powerfully galvanizing forces shaping history in the world today is the prophecy of Gog and Magog from the 38th and 39th chapters of the book of Ezekiel. This prophecy from the Jewish-Christian Bible has molded geo-politics, not only with- in the United States and the West but also, to an amazing degree, in the Muslim world as well. It seems that, millennia ago, Ezekiel’s vision actually named the nation which millions today believe plays the major role in this prophecy: the nation of Russia. Many modern scholars have dismissed Ezekiel’s Gog and Magog prophecy as a mystical apocalypse written to vindicate the ancient claims of a minor country’s deity. The very notion of such a prediction—that semi-mythical and unrelated nations that dwelt on the fringes of Israel’s geographical consciousness 2,500 years ago would, “in the latter days,” suddenly coalesce into a tidal wave of opposition to a newly regathered state of Jews—seems utterly incredible to a modern mentality. Such a scenario, the experts say, belongs only to the fundamentalist “pop religion” of The Late, Great Planet Earth and of TV evangelists. -
Peter Weiss. Andrei Platonov. Ragnvald Blix. Georg Henrik Von Wright. Adam Michnik
A quarterly scholarly journal and news magazine. March 2011. Vol IV:1 From the Centre for Baltic and East European Studies (CBEES) Södertörn University, Stockholm FEATURE. Steklov – Russian BALTIC temple of pure thought W O Rbalticworlds.com L D S COPING WITH TRANSITIONS PETER WEISS. ANDREI PLATONOV. RAGNVALD BLIX. GEORG HENRIK VON WRIGHT. ADAM MICHNIK. SLAVENKA DRAKULIĆ. Sixty pages BETRAYED GDR REVOLUTION? / EVERYDAY BELARUS / WAVE OF RELIGION IN ALBANIA / RUSSIAN FINANCIAL MARKETS 2short takes Memory and manipulation. Transliteration. Is anyone’s suffering more important than anyone else’s? Art and science – and then some “IF YOU WANT TO START a war, call me. Transliteration is both art and science CH I know all about how it's done”, says – and, in many cases, politics. Whether MÄ author Slavenka Drakulić with a touch царь should be written as tsar, tzar, ANNA of gallows humor during “Memory and czar, or csar may not be a particu- : H Manipulation: Religion as Politics in the larly sensitive political matter today, HOTO Balkans”, a symposium held in Lund, but the question of the transliteration P Sweden, on December 2, 2010. of the name of the current president This issue of the journal includes a of Belarus is exceedingly delicate. contribution from Drakulić (pp. 55–57) First, and perhaps most important: in which she claims that top-down gov- which name? Both the Belarusian ernance, which started the war, is also Аляксандр Лукашэнка, and the Rus- the path to reconciliation in the region. sian Александр Лукашенко are in use. Balkan experts attending the sympo- (And, while we’re at it, should that be sium agree that the war was directed Belarusian, or Belarussian, or Belaru- from the top, and that “top-down” is san, or Byelorussian, or Belorussian?) the key to understanding how the war BW does not want to take a stand on began in the region. -
Identification of Buried Lunar Impact Craters from GRAIL Data And
PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Identification of buried lunar impact craters from GRAIL 10.1002/2015GL067394 data and implications for the nearside maria Key Points: Alexander J. Evans1,2,3, Jason M. Soderblom1, Jeffrey C. Andrews-Hanna4, Sean C. Solomon2,5, • One-hundred four buried crater 1 candidates on the lunar nearside are and Maria T. Zuber fi identi ed from gravity anomalies 1 • The density, thickness, and volume of Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, 2 3 infilling deposits are determined Massachusetts, USA, Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York, USA, Now at Planetary Science Directorate, Southwest Research Institute, Boulder, Colorado, USA, 4Planetary Science Directorate, Southwest Research Institute, Boulder, Colorado, USA, 5Department of Terrestrial Magnetism, Carnegie Institution of Supporting Information: • Figures S1–S7 and Table S1 and S2 Washington, Washington, District of Columbia, USA Caption • Table S1 • Table S2 Abstract Gravity observations from the dual Gravity Recovery and Interior Laboratory (GRAIL) spacecraft have revealed more than 100 quasi-circular mass anomalies, 26–300 km in diameter, on the lunar nearside. Correspondence to: These anomalies are interpreted to be impact craters filled primarily by mare deposits, and their characteristics A. J. Evans, fl [email protected] are consistent with those of impact structures that formed prior to, and during, intervals of ooding of feldspathic terrane by mare basalt lavas. We determine that mare deposits have an average density contrast of þ300 À3 850À kg m relative to the surrounding crust. The presence of a large population of volcanically buried Citation: 200 Evans,A.J.,J.M.Soderblom,J.C.Andrews- craters with minimal topographic expression and diameters up to 300 km requires an average nearside mare Hanna, S. -
Amagmatic Hydrothermal Systems on Mars from Radiogenic Heat ✉ Lujendra Ojha 1 , Suniti Karunatillake 2, Saman Karimi 3 & Jacob Buffo4
ARTICLE https://doi.org/10.1038/s41467-021-21762-8 OPEN Amagmatic hydrothermal systems on Mars from radiogenic heat ✉ Lujendra Ojha 1 , Suniti Karunatillake 2, Saman Karimi 3 & Jacob Buffo4 Long-lived hydrothermal systems are prime targets for astrobiological exploration on Mars. Unlike magmatic or impact settings, radiogenic hydrothermal systems can survive for >100 million years because of the Ga half-lives of key radioactive elements (e.g., U, Th, and K), but 1234567890():,; remain unknown on Mars. Here, we use geochemistry, gravity, topography data, and numerical models to find potential radiogenic hydrothermal systems on Mars. We show that the Eridania region, which once contained a vast inland sea, possibly exceeding the combined volume of all other Martian surface water, could have readily hosted a radiogenic hydro- thermal system. Thus, radiogenic hydrothermalism in Eridania could have sustained clement conditions for life far longer than most other habitable sites on Mars. Water radiolysis by radiogenic heat could have produced H2, a key electron donor for microbial life. Furthermore, hydrothermal circulation may help explain the region’s high crustal magnetic field and gravity anomaly. 1 Department of Earth and Planetary Sciences. Rutgers, The State University of New Jersey, Piscataway, NJ, USA. 2 Department of Geology and Geophysics, Louisiana State University, Baton Rouge, LA, USA. 3 Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA. 4 Thayer ✉ School of Engineering, Dartmouth College, Hanover, NH, USA. email: [email protected] NATURE COMMUNICATIONS | (2021) 12:1754 | https://doi.org/10.1038/s41467-021-21762-8 | www.nature.com/naturecommunications 1 ARTICLE NATURE COMMUNICATIONS | https://doi.org/10.1038/s41467-021-21762-8 ydrothermal systems are prime targets for astrobiological for Proterozoic crust)44. -
A Sedimentary Origin for Intercrater Plains North of the Hellas Basin
A sedimentary origin for intercrater plains north of the Hellas basin: Implications for climate conditions and erosion rates on early Mars Francesco Salese, Veronique Ansan, Nicolas Mangold, John Carter, Anouck Ody, François Poulet, Gian Gabriele Ori To cite this version: Francesco Salese, Veronique Ansan, Nicolas Mangold, John Carter, Anouck Ody, et al.. A sedimentary origin for intercrater plains north of the Hellas basin: Implications for climate conditions and erosion rates on early Mars. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2016, 121 (11), pp.2239-2267. 10.1002/2016JE005039. hal-02305998 HAL Id: hal-02305998 https://hal.archives-ouvertes.fr/hal-02305998 Submitted on 4 Oct 2019 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. PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE A sedimentary origin for intercrater plains north of the Hellas 10.1002/2016JE005039 basin: Implications for climate conditions Key Points: and erosion rates on early Mars • Intercrater plains on the northern rim of Hellas basin are -
Geophysical Evolution of Planetary Interiors and Surfaces: Moon & Mars -MASSACHUI by Alexander Joseph Evans OCT B.S.E., University of Michigan (2006) F R Slt
Geophysical Evolution of Planetary Interiors and Surfaces: Moon & Mars -MASSACHUI by Alexander Joseph Evans OCT B.S.E., University of Michigan (2006) F r Slt Submitted to the Department of Earth, Atmospheric and Planetary Sciences in partial fulfillment of the requirements for the degree of Doctor of Philosophy at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY September 2013 @ Massachusetts Institute of Technology 2013. All rights reserved. /f A uthor ... .. .. .. ..... ... C..1... .. .. ... .. ..... Deqartment of Earth, Atmospheric and Planetary Sciences September 6, 2013 Certified by ...... .... ................... Maria T. Zuber E. A. Griswold Professor of Geophysics 72 Thesis Supervisor Accepted by.......- ---- ..... Robert D. van der Hilst Schlumberger Professor of Earth Sciences Head, Department of Earth, Atmospheric and Planetary Sciences Geophysical Evolution of Planetary Interiors and Surfaces: Moon & Mars by Alexander Joseph Evans Submitted to the Department of Earth, Atmospheric and Planetary Sciences on September 6, 2013, in partial fulfillment of the requirements for the degree of Doctor of Philosophy Abstract The interiors and surfaces of the terrestrial planetary bodies provide us a unique opportu- nity to gain insight into planetary evolution, particularly in the early stages subsequent to accretion. Both Mars and the Moon are characterized by well-preserved and ancient sur- faces, that preserve a record of geological and geophysical processes that have operated both at the surface and in the interior. With accessibility to orbital and landed spacecraft, the Moon and Mars have a unique qualitative and quantitative role in understanding and constraining the evolution of solid planets in our Solar System, as well as the timing of its many major events. In this thesis I use gravity and topography data to investigate aspects of the surface and interior evolution of the Moon and Mars that include aspects of major processes: impact, volcanism, erosion and internal dynamics. -
Morphology and Origin of Lunar Craters Von R
Morphology and origin of lunar craters Von R. S. Saunders, E. L. Haines, and J. E. Conel, Pasaderia" Summary: The general concensus among lunar geologists is th.at the majority of lunar craters, up to a few km in diameter, are of Impact origm. This conclusion is based on morphologie comparison with terrestrial meteorite craters, consideration of lunar regolrth formation by impact, direct observation of the morphology of smalI and microscopic craters on the lunar surface and experimental impact studtcs. Most Iarge craters are also interpreted to be ()f Impact origin. Although the morphology of unmodified craters changes somewhat with increasing size, these changes are completely gradational and there is no evidence to suggest that the predominant process of crater formation is different for large craters. However, selected craters of various sizes have been interpreted as volcanic. Understanding the origm of the multi-ring b asms presents greater difficulties. Theoretical treatments such as those of Bjork (1961) and Van Dorn (1969) seem to be the only approach. In such treatments it is nccessary to iriclude, in addition to hydrodynamic flow, large plastrc deformation arid br.it.tle failure of the target material, processes that are known to accompany Impact phenomena. Thus complete equations of state are required as well as a detailed microscopic (perhaps statistical) description of imperfections in rock mechanical properties. The required physical parameters arid the calculations are clearly formidable. Analysis of tracking data from Orbiter V has revealed positive graviational anomalies (mascons) over the circular maria (Mulle r und Sjogren, 1968). While a number of theories for the origin of the mascons has been proposed (see Kaula, 1969 for a summary), the nature of the anomalous masses remains in doubt as does the mechamsm whereby excess mass has been added to specific rcgtons, Resolution of these questions will tell us much about the thermal and struc tural history of the Moon. -
A Model for the Climatic Behavior of Water on Mars. Stephen Mark Clifford University of Massachusetts Amherst
University of Massachusetts Amherst ScholarWorks@UMass Amherst Doctoral Dissertations 1896 - February 2014 1-1-1984 A model for the climatic behavior of water on Mars. Stephen Mark Clifford University of Massachusetts Amherst Follow this and additional works at: https://scholarworks.umass.edu/dissertations_1 Recommended Citation Clifford, Stephen Mark, "A model for the climatic behavior of water on Mars." (1984). Doctoral Dissertations 1896 - February 2014. 1781. https://scholarworks.umass.edu/dissertations_1/1781 This Open Access Dissertation is brought to you for free and open access by ScholarWorks@UMass Amherst. It has been accepted for inclusion in Doctoral Dissertations 1896 - February 2014 by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. A MODEL FOR THE CLIMATIC BEHAVIOR OF WATER ON MARS. A Dissertation Presented By STEPHEN MARK CLIFFORD the Submitted to the Graduate School of fulfillment University of Massachusetts in partial degree of of the requirements for the DOCTOR OF PHILOSOPHY May 1984 Department of Physics and Astronomy Stephen Mark Clifford All Rights Reserved Space Administration National Aeronautics and NSG 7405 11 n A MODEL FOR THE CLIMATIC BEHAVIOR OF WATER ON MARS. A Dissertation Presented By STEPHEN MARK CLIFFORD Approved as to style and content by: up Robert L. Hug uen i Chairperson/ of Committee Daniel Hillel, Member William M. Irvine, Member George (|/. McGill, Member / Head LeRoy F. Cook, Department Department of Physics and Astronomy iii DEDICATION support I would have To ny wife, Julie, without whose love and given all this up long ago. iv ACKNOWLEDGEMENTS Robert Huguenin, who stimulated I am deeply indebted to Professor His creativity, support, and encouraged much of my graduate research.