DOCSLIB.ORG

Using Ground-Failure Features for Paleoseismic Analysis

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Using Ground-Failure Features for Paleoseismic Analysis USING GROUND-FAILURE FEATURES FOR PALEOSEISMIC ANALYSIS Stephen F. Obermeier and Randall W. Jibson, editors USING UQUEFACTION-INDUCED FEATURES FOR PALEOSEISMIC ANALYSIS Chapter A, by Stephen F. Obermeier USING LANDSLIDES FOR PALEOSEISMIC ANALYSIS Chapter B, by Randall W. Jibson U.S. Geological Survey Open-File Report 94-663 This report has not been reviewed for conformity with U. S. Geological Survey editorial standards. Use of brand names in this report is for the sake of description. ACKNOWLEDGMENT Funding for much of the research required for this report was provided by the Earthquake Hazards and Landslide Hazards Programs of the U. S. Geological Survey, as well as by grants from the U. S. Nuclear Regulatory Commission. The Charter A manuscript recieved constructive reviews from John Sims, Alan Nelson, Tom Holzer, Randall Jibson, and Eugene Schweig of the U. S. Geological Survey, from T. Leslie Youd of Brigham Young University, and from Martitia Tuttle of the University of Maryland. Chapter B recieved helpful reviews from Robert Schuster of the U. S. Geological Survey, and from Jim McCalpin of GEO-HAZ, Inc. PREFACE Faults are not exposed at the ground surface or are unavailable for study in many tectonic environments. Therefore other types of geologic evidence are required to reconstruct the prehistoric seismic record of an area. Seismic shaking can produce many different types of ground deformation that can be preserved in the geologic record. Many of the types are discussed in the two papers following, but the papers focus primarily on (1) seismically induced liquefaction features and (2) landslides that move as coherent blocks (slumps and block slides) during seismic shaking. Analysis of both liquefaction-induced features and coherent landslides permits quantitative estimation of levels of prehistoric shaking in many field situations. Most other types of deformations permit only crude estimates of shaking levels. Liquefaction-induced features such as sand-filled fissures are also important because they form only in fairly high levels of seismic shaking: the minimum moment magnitude is about 5.5- 6.0 in most geologic environments. Presence of the sand-filled fissures indicates earthquakes that would have damaged built structures. For landslides, the minimum magnitude is somewhat smaller, about 4.5-5.0 for many types of landslides. Proving a seismic origin for liquefaction-induced features is not very difficult in many geologic environments, particularly where past seismic shaking has been very strong. Independent lines of evidence generally are not required for a definitive assessment of origin. Demonstrating a seismic origin generally involves excluding only a few possible alternate sources for fluidizing sediments, and criteria for doing so have been developed that can be applied to many field situations. Determining a seismic origin for landslides is much more difficult because of the broader range of conditions that can lead to slope failure. Thus, for landslides, multiple, independent lines of evidence of seismic origin generally are required. Paleoseismic ground-failure studies differ fundamentally from paleoseismic fault studies. Whereas fault studies seek to characterize the movement history of a specific fault, ground-failure studies characterize the shaking history of a site or region irrespective of the earthquake source. In regions that contain multiple seismic sources and in regions where faults cannot be studied in detail, which are the norm, paleoseismic ground-failure studies can be particularly valuable tools in hazard and risk assessments. The approaches discussed in these two papers have evolved largely within the past 10 years. The techniques have already been instrumental in greatly advancing the status of knowledge about prehistoric seismicity in diverse regions and geologic settings. In addition, the techniques permit estimation of prehistoric levels of shaking and earthquake magnitude in some cases, which can make the techniques at least as useful as fault studies for gleaning information about paleoseismicity. Stephen F. Obermeier and Randall W. Jibson, editors CHAPTER A USING LIQUEFACTION-INDUCED FEATURES FOR PALEOSEISMIC ANALYSIS STEPHEN F. OBERMEIER U. S. GEOLOGICAL SURVEY OPEN-FILE REPORT 94-663 CHAPTER A CONTENTS ABSTRACT 1. INTRODUCTION 2. OVERVIEW OF THE FORMATION OF LIQUEFACTION- INDUCED FEATURES 2.1 Process of liquefaction and fluidization 2.2 Factors affecting liquefaction susceptibility and fluidization 2.2.1 grain size 2.2.2 relative density 2.2.3 depth of ground-water table 2.2.4 depth and thickness of strata 2.2.5 site effects and nature of seismic shaking 2.2.6 geologic details of the cap 2.2.7 seismic history 2.2.8 age and mineralogy of sediments 3. CRITERIA FOR AN EARTHQUAKE-INDUCED LIQUEFACTION ORIGIN 4. HISTORIC AND PREHISTORIC LIQUEFACTION-SELECTED STUDIES 4.1 Coastal South Carolina 4.1.1 characterization of craters 4.1.2 prehistoric seismicity 4.2 New Madrid Seismic Zone 4.2.1 characterization of venting and fracturing at the ground surface 4.2.2 characterization of sand blows and dikes in sectional view 4.2.3 characterization of sills in sectional view 4.2.4 paleoliquefaction studies 4.3 Wabash Valley Seismic Zone 4.3.1 characterization of features 4.3.2 ages of dikes 4.3.3 evidence for seismic origin 4.3.4 paleoseismic implications 4.4 Coastal Washington 4.4.1 Columbia River features 4.4.2 strength of prehistoric shaking 4.4.3 ancient marine terrace features 5. FEATURES GENERALLY OF NONSEISMIC OR UNKNOWN ORIGIN 5.1 Terrestrial disturbance features 5.1.1 nonseismic sand boils 5.1.2 streambank landslides 5.1.3 ground disturbance by trees 5.1.4 mima mounds 5.2 Features formed in subaqueous environments 5.2.1 load structures in muds 5.2.2 water-escape features in granular sediments 5.2.3 sheet slumps, warped beds, and recumbent folds 5.2.4 turbidity flow features 5.2.5 paleoseismic examples 5.3 Features formed by weathering 5.4 Features formed in a periglacial environment 5.4.1 involutions 5.4.2 ice-wedge casts 6. ESTIMATION OF STRENGTH OF PALEOEARTHQUAKES 6.1 Association with Modified Mercalli Intensity 6.2 Magnitude bound 6.3 Method of Seed and Idriss 6.4 Overview of estimates of magnitude 6.5 Negative evidence CHAPTER A USING LIQUEFACTION-INDUCED FEATURES FOR PALEOSEKMIC ANALYSIS STEPHEN F. OBERMEIER U. S. Geological Survey 922 National Center Reston, Virginia, 22092 ABSTRACT Liquefaction features can be used in many field settings to estimate the recurrence interval and magnitude of strong earthquakes through much of the Holocene. The relatively high shaking level required for their formation makes them particularly valuable as records of strong paleo-earthquakes. This state-of-the-art summary for interpretation and analysis of liquefaction effects takes into account input from both geologic and geotechnical engineering perspectives. Discussed are an overview of the processes involved in formation of the features, criteria for determining whether sediments have been deformed by seismically induced liquefaction, case studies in various geologic settings, and description of the methods for estimating magnitude of prehistoric earthquakes. Also discussed are some types of sediment deformations that can be misinterpreted as having a seismic origin. 1. INTRODUCTION This text focuses on the methodology for determining whether observed sediment deformation had a seismic shaking origin or a nonseismic origin. Emphasis is placed on the process of liquefaction, which is the transformation of a granular material from a solid state into a liquefied state as a consequence of increased pore-water pressures (Youd, 1973). The discussion encompasses various manifestations of liquefaction-induced deformation in fluvial and nearshore-marine deposits, and the application of criteria for establishing an earthquake origin. The systematic study of paleoliquefaction is a young discipline. Accordingly, some of the physical parameters that control effects of liquefaction in the field are not completely understood. Still, the principles and methodology for conducting paleoliquefaction studies are sufficiently advanced to warrant their routine application in paleoseismic studies. The method in this text for conducting paleoliquefaction studies was developed largely out of necessity in the United States, where the historic seismic record is particularly short. Paleoliquefaction studies are useful to engineers and planners because of the high shaking threshold required to develop liquefaction features. The threshold is a horizontal acceleration on the order of 0.1 g for strong earthquakes, even in highly susceptible sediment (National Research Council, 1985, p. 34; Ishihara, 1985, p. 352). Worldwide data on historical earthquakes show that features having a liquefaction origin can be developed at earthquake magnitudes as low as about 5, but that a magnitude of about 5.5 to 6 is the lower limit at which liquefaction effects become relatively common (Ambraseys, 1988). (Earthquake magnitude, M, is used rather loosely as either moment magnitude or surface- wave magnitude, whichever is larger.) Liquefaction has been severe and widespread in many worldwide earthquakes. Effects of liquefaction have many manifestations. Some noteworthy reports discuss the effects in the region of the 1811-12 New Madrid, Missouri, earthquakes (Fuller, 1912), in the region of the 1886 Charleston, South Carolina, earthquake (Dutton, 1889), in northern California (Youd and Hoose, 1978), in the vicinity of the 1964 Alaska earthquake
Load more

Recommended publications
  • JPL to Map the Moon on India Mission
    I n s i d e May 19, 2006 Volume 36 Number 10 News Briefs ............... 2 Griffin Visits Lab ............ 3 Special Events Calendar ...... 2 Passings, Letters ........... 4 Spitzer Sees Comet Breakup... 2 Retirees, Classifieds ......... 4 Jet Propulsion Laborator y A JPL state-of-the-art imaging spectrometer that will provide the first high-resolution spectral map of the JPL to entire lunar surface successfully completed its critical design review this week. The Moon Mineralogy Mapper, also known as “M3,” is one of two in- materials across the surface at high spatial resolution. This data map the struments that NASA is contributing to India’s first mission to the moon, will provide a much-needed long-term baseline for future exploration scheduled to launch in late 2007 or early 2008. By mapping the mineral activities. composition of the lunar surface, the mission will both provide clues to The mission’s observations will address several important scientific moon the early development of the solar system and guide future astronauts to issues, including early evolution of the solar system; fundamental stores of precious resources. processes acting on planets that shape their character; assessment of on India Chandrayaan-1 is India’s first deep-space mission as well as its first potential impact hazards to Earth; and assessment of space resources. lunar mission. “The entire M3 team feels honored to be able to partici- From its vantage point in orbit around the moon, the spacecraft will mission pate,” said Project Manager Tom Glavich of JPL. measure the sunlight reflected by all of the rocks and soil over which The instrument is well on its way to being delivered to the Chandray- it passes.
    [Show full text]
  • GRAIL Reveals Secrets of the Lunar Interior
    GRAIL Reveals Secrets of the Lunar Interior — Dr. Patrick J. McGovern, Lunar and Planetary Institute A mini-flotilla of spacecraft sent to the Moon in the past few years by several nations has revealed much about the characteristics of the lunar surface via techniques such as imaging, spectroscopy, and laser ranging. While the achievements of these missions have been impressive, only GRAIL has seen deeply enough to reveal inner secrets that the Moon holds. LRecent Lunar Missions Country Name Launch Date Status ESA Small Missions for Advanced September 27, 2003 Ended with lunar surface impact on Research in Technology-1 (SMART-1) September 3, 2006 USA Acceleration, Reconnection, February 27, 2007 Extension of the THEMIS mission; ended Turbulence and Electrodynamics of in 2012 the Moon’s Interaction with the Sun (ARTEMIS) Japan SELENE (Kaguya) September 14, 2007 Ended with lunar surface impact on June 10, 2009 PChina Chang’e-1 October 24, 2007 Taken out of orbit on March 1, 2009 India Chandrayaan-1 October 22, 2008 Two-year mission; ended after 315 days due to malfunction and loss of contact USA Lunar Reconnaissance Orbiter (LRO) June 18, 2009 Completed one-year primary mission; now in five-year extended mission USA Lunar Crater Observation and June 18, 2009 Ended with lunar surface impact on Sensing Satellite (LCROSS) October 9, 2009 China Chang’e-2 October 1, 2010 Primary mission lasted for six months; extended mission completed flyby of asteroid 4179 Toutatis in December 2012 USA Gravity Recovery and Interior September 10, 2011 Ended with lunar surface impact on I Laboratory (GRAIL) December 17, 2012 To probe deeper, NASA launched the Gravity Recovery and Interior Laboratory (GRAIL) mission: twin spacecraft (named “Ebb” and “Flow” by elementary school students from Montana) flying in formation over the lunar surface, tracking each other to within a sensitivity of 50 nanometers per second, or one- twenty-thousandth of the velocity that a snail moves [1], according to GRAIL Principal Investigator Maria Zuber of the Massachusetts Institute of Technology.
    [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]
  • Strategies for Detecting Biological Molecules on Titan
    ASTROBIOLOGY Volume 18, Number 5, 2018 ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2017.1758 Strategies for Detecting Biological Molecules on Titan Catherine D. Neish,1 Ralph D. Lorenz,2 Elizabeth P. Turtle,2 Jason W. Barnes,3 Melissa G. Trainer,4 Bryan Stiles,5 Randolph Kirk,6 Charles A. Hibbitts,2 and Michael J. Malaska5 Abstract Saturn’s moon Titan has all the ingredients needed to produce ‘‘life as we know it.’’ When exposed to liquid water, organic molecules analogous to those found on Titan produce a range of biomolecules such as amino acids. Titan thus provides a natural laboratory for studying the products of prebiotic chemistry. In this work, we examine the ideal locales to search for evidence of, or progression toward, life on Titan. We determine that the best sites to identify biological molecules are deposits of impact melt on the floors of large, fresh impact craters, specifically Sinlap, Selk, and Menrva craters. We find that it is not possible to identify biomolecules on Titan through remote sensing, but rather through in situ measurements capable of identifying a wide range of biological molecules. Given the nonuniformity of impact melt exposures on the floor of a weathered impact crater, the ideal lander would be capable of precision targeting. This would allow it to identify the locations of fresh impact melt deposits, and/or sites where the melt deposits have been exposed through erosion or mass wasting. Determining the extent of prebiotic chemistry within these melt deposits would help us to understand how life could originate on a world very different from Earth.
    [Show full text]
  • Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America
    Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America There are approximately 101,135sexual abuse claims filed. Of those claims, the Tort Claimants’ Committee estimates that there are approximately 83,807 unique claims if the amended and superseded and multiple claims filed on account of the same survivor are removed. The summary of sexual abuse claims below uses the set of 83,807 of claim for purposes of claims summary below.1 The Tort Claimants’ Committee has broken down the sexual abuse claims in various categories for the purpose of disclosing where and when the sexual abuse claims arose and the identity of certain of the parties that are implicated in the alleged sexual abuse. Attached hereto as Exhibit 1 is a chart that shows the sexual abuse claims broken down by the year in which they first arose. Please note that there approximately 10,500 claims did not provide a date for when the sexual abuse occurred. As a result, those claims have not been assigned a year in which the abuse first arose. Attached hereto as Exhibit 2 is a chart that shows the claims broken down by the state or jurisdiction in which they arose. Please note there are approximately 7,186 claims that did not provide a location of abuse. Those claims are reflected by YY or ZZ in the codes used to identify the applicable state or jurisdiction. Those claims have not been assigned a state or other jurisdiction. Attached hereto as Exhibit 3 is a chart that shows the claims broken down by the Local Council implicated in the sexual abuse.
    [Show full text]
  • September GEM Newsletter
    March 2015 GEM Volume 3, Issue GEM God Everyone Me GEM is the official publication of the St. Charles Borromeo Council of the Knights of Columbus. It is published monthly by Knights of Columbus Council #3960, Randallstown, MD 21133, with an average circulation of approximately 160. Inquiries should be directed to the Editor. Grand Knight’s Message INSIDE THIS ISSUE Grand Knight’s Message 1 Chaplin’s Message 1 Brother Knights, Activities 2 Birthdays 3 I hope everyone is surviving the relentless District Deputy[s Report 4 Good of the Order 5 winter of 2014-15. Growing up in Lottery Winners 6 Pennsylvania, I remember many cold, snowy Feature 7 winters, but none like this past month Bingo Schedules 9 (maybe I am getting old). As we continue our Lenten journey, I would like to offer the words of Saint John Paul II in his Lenten intellectually. Do our actions really indicate message of 2003, “It is my fervent hope belief in the gospel, in God and His son, that believers will find this Lent a favorable Jesus Christ? Do our external penances time for bearing witness to the Gospel of really reflect true belief, or, are they like charity in every place, since the vocation to some of the sacrifices of the Old Testament charity is the heart of all true in which the people often “honored God evangelization.” Following his words, pick a with their lips but their heart was far from charity to either make a monetary donation, Him,” as the Prophet Isaiah s complained. or give of yourself, which would be more meaningful.
    [Show full text]
  • 304 Index Index Index
    _full_alt_author_running_head (change var. to _alt_author_rh): 0 _full_alt_articletitle_running_head (change var. to _alt_arttitle_rh): 0 _full_article_language: en 304 Index Index Index Adamson, Robert (1821–1848) 158 Astronomische Gesellschaft 216 Akkasbashi, Reza (1843–1889) viiii, ix, 73, Astrolog 72 75-78, 277 Astronomical unit, the 192-94 Airy, George Biddell (1801–1892) 137, 163, 174 Astrophysics xiv, 7, 41, 57, 118, 119, 139, 144, Albedo 129, 132, 134 199, 216, 219 Aldrin, Edwin Buzz (1930) xii, 244, 245, 248, Atlas Photographique de la Lune x, 15, 126, 251, 261 127, 279 Almagestum Novum viii, 44-46, 274 Autotypes 186 Alpha Particle Spectrometer 263 Alpine mountains of Monte Rosa and BAAS “(British Association for the Advance- the Zugspitze, the 163 ment of Science)” 26, 27, 125, 128, 137, Al-Biruni (973–1048) 61 152, 158, 174, 277 Al-Fath Muhammad Sultan, Abu (n.d.) 64 BAAS Lunar Committee 125, 172 Al-Sufi, Abd al-Rahman (903–986) 61, 62 Bahram Mirza (1806–1882) 72 Al-Tusi, Nasir al-Din (1202–1274) 61 Baillaud, Édouard Benjamin (1848–1934) 119 Amateur astronomer xv, 26, 50, 51, 56, 60, Ball, Sir Robert (1840–1913) 147 145, 151 Barlow Lens 195, 203 Amir Kabir (1807–1852) 71 Barnard, Edward Emerson (1857–1923) 136 Amir Nezam Garusi (1820–1900) 87 Barnard Davis, Joseph (1801–1881) 180 Analysis of the Moon’s environment 239 Beamish, Richard (1789–1873) 178-81 Andromeda nebula xii, 208, 220-22 Becker, Ernst (1843–1912) 81 Antoniadi, Eugène M. (1870–1944) 269 Beer, Wilhelm Wolff (1797–1850) ix, 54, 56, Apollo Missions NASA 32, 231, 237, 239, 240, 60, 123, 124, 126, 130, 139, 142, 144, 157, 258, 261, 272 190 Apollo 8 xii, 32, 239-41 Bell Laboratories 270 Apollo 11 xii, 59, 237, 240, 244-46, 248-52, Beg, Ulugh (1394–1449) 63, 64 261, 280 Bergedorf 207 Apollo 13 254 Bergedorfer Spektraldurchmusterung 216 Apollo 14 240, 253-55 Biancani, Giuseppe (n.d.) 40, 274 Apollo 15 255 Biot, Jean Baptiste (1774–1862) 1,8, 9, 121 Apollo 16 240, 255-57 Birt, William R.
    [Show full text]
  • 2 / Lunar Base Concepts
    2 / LUNAR BASE CONCEPTS HE TERM "LUNAR BASE" can refer to a spectrum of concepts ranging from a mannable "line shack" to a multifunctional, self-sufficient, populous Tcolony. In general, the authors contributing to this book discuss the earliest stages of a permanently manned facility with the capability for scientific investigations and some ability to support its own operation with local materials. The exact form of the "final" configuration usually is not critical to the discussion until cost is included. Costs of a lunar base can be similar to the space station program or can be at the level of the Apollo project. Since cost is such a sensitive topic in the advocacy phase, it becomes very important to understand not only the total cost but also the spending rate and the basic assumptions about what is charged to the project. The costs derived by Hoffman and Niehoff in their study presented in this section differ from costs referenced by Sellers and Keaton in a later section. The final configurations in the two studies differ considerably, but in both cases the spending rates over the duration of the project are well within the rate of expenditure of the current space program and are substantially less than rates associated with Project Apollo. Because lower cost is a major strategy goal, design concepts generally adopt hardware from prior programs. For example, the studies conducted by NASA in the 1960's and described by Lowrnan and by Johnson and Leonard depict habitats inspired by the Apollo transportation system. Contemporary drawings show space station modules emplaced on the lunar surface.
    [Show full text]
  • Characterization of Previously Unidentified Lunar Pyroclastic Deposits Using Lunar Reconnaissance Orbiter Camera Data J
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00H25, doi:10.1029/2011JE003893, 2012 Characterization of previously unidentified lunar pyroclastic deposits using Lunar Reconnaissance Orbiter Camera data J. Olaf Gustafson,1 J. F. Bell III,2,3 L. R. Gaddis,4 B. R. Hawke,5 and T. A. Giguere5,6 Received 1 July 2011; revised 31 March 2012; accepted 14 April 2012; published 8 June 2012. [1] We used a Lunar Reconnaissance Orbiter Camera (LROC) global monochrome Wide-angle Camera (WAC) mosaic to conduct a survey of the Moon to search for previously unidentified pyroclastic deposits. Promising locations were examined in detail using LROC multispectral WAC mosaics, high-resolution LROC Narrow Angle Camera (NAC) images, and Clementine multispectral (ultraviolet-visible or UVVIS) data. Out of 47 potential deposits chosen for closer examination, 12 were selected as probable newly identified pyroclastic deposits. Potential pyroclastic deposits were generally found in settings similar to previously identified deposits, including areas within or near mare deposits adjacent to highlands, within floor-fractured craters, and along fissures in mare deposits. However, a significant new finding is the discovery of localized pyroclastic deposits within floor-fractured craters Anderson E and F on the lunar farside, isolated from other known similar deposits. Our search confirms that most major regional and localized low-albedo pyroclastic deposits have been identified on the Moon down to 100 m/pix resolution, and that additional newly identified deposits are likely to be either isolated small deposits or additional portions of discontinuous, patchy deposits. Citation: Gustafson, J. O., J. F. Bell III, L. R. Gaddis, B.
    [Show full text]
  • The Space Race Documented Through Front Pages of Newspapers from Around North America
    The News Frontier The Space Race documented through front pages of newspapers from around North America Newspapers and patches generously donated to the McAuliffe-Shepard Discovery Center by Jerrid Kenney After the end of World War II, a new battle began: the Cold War. In the mid-20th century, the United States and the Soviet Union were each trying to prove they were better than the other. Both sides wanted to show the superiority of their technology, military, and, by extension, their political systems. Starting in the late 1950s, the battlefront reached space. The United States and the Soviet Union fought to first achieve milestones in space exploration—starting in 1957 with the Soviet Union’s launch of Sputnik I, continuing through the U.S.’s landing astronauts on the Moon in 1969, and ending with a handshake in space between American astronauts and Soviet cosmonauts in 1975. Witness the fight for extraterrestrial might by reading about the United States and the Soviet Union’s major feats of the Space Race, as recorded in American and Canadian newspapers in real time. The Space Race Over Time July 15-24, 1975 February 20, 1962 May 28, 1964 The Space Race comes October 4, 1957 April 12, 1961 July 20, 1969 John Glenn becomes NASA launches to an end with the Soviet Union Yuri Gagarin Neil Armstrong first American to unmanned Saturn I Apollo-Soyuz Test launches first becomes first becomes the first orbit the Earth rocket as first step Project, the in-orbit artificial satellite human in space human to walk on of the Apollo the Moon docking of U.S.
    [Show full text]
  • REFERENCES LUNAR SAMPLE COMPENDIUM (July 2012)
    REFERENCES LUNAR SAMPLE COMPENDIUM (July 2012) Note: The abstract volumes of the annual Lunar Science and Lunar and Planetary Science Conferences were issued by the Lunar and Planetary Science Institute, Houston.. Initially, the Proceedings of these annual conferences were supplements to Geochim. Cosmochim. Acta (volumes 1-12), later J. Geophys. Res.(volumes 13-17). Proceedings 18-22 were produced and published by the Lunar Planetary Science Institute. There is an index to the first nine Lunar Science Conferences (Masterson 1979). Proceedings papers were peer-reviewed, while abstracts were not. Abell P.I., Cadogen P.H., Eglington G., Maxwell J.R. and Pillinger C.T. (1971) Survey of lunar carbon compounds. Proc. Second Lunar Sci. Conf. 1843-1863. Abu-Eid R.M., Vaughan D.J., Whitner M., Burns R.G. and Morawski A. (1973) Spectral data bearing on the oxidation states of Fe, Ti, and Cr in Apollo 15 and Apollo 16 samples (abs). Lunar Sci. IV, 1-3. Lunar Planetary Institute, Houston. Adams J.B. and McCord T.B. (1970) Remote sensing of lunar surface mineralogy: Implications from visible and near-infrared reflectivity of Apollo 11 samples. Proc. Apollo 11 Lunar Sci. Conf. 1937-1946. Adams J.B. and McCord T.B. (1971) Optical properties of mineral separates, glass and anorthosite fragments from Apollo mare samples. Proc. Second Lunar Sci. Conf. 2183-2195. Adams J.B. and McCord T.B. (1972) Optical evidence for average pyroxene composition of Apollo 15 samples. In The Apollo 15 Lunar Samples, 10-13. Lunar Planetary Institute, Houston. Adams J.B. and McCord T.B.
    [Show full text]
  • Lunar Sourcebook : a User's Guide to the Moon
    REFERENCES Adams J. B. (1974) Visible and near-infrared diffuse chemistry, mineralogy and petrology of some Apollo 11 reflectance spectra of pyroxenes as applied to remote lunar samples. Proc. Apollo 11 Lunar Sci. Conf., pp. 93–128. sensing of solid objects in the solar system. J. Geophys. Ahrens T. J. and Cole D. M. (1974) Shock compression and Res., 79, 4829–4836. adiabatic release of lunar fines from Apollo 17. Proc. Lunar Adams J. B. (1975) Interpretation of visible and near-infrared Sci. Conf. 5th, pp. 2333–2345. diffuse reflectance spectra of pyroxenes and other rock Ahrens T. J. and O’Keefe J. D. (1977) Equations of state and forming minerals. In Infrared and Raman Spectroscopy of impact-induced shock-wave interaction on the Moon. In Lunar and Terrestrial Materials (C. Karr, ed.), pp. 91–116. Impact and Explosion Cratering (D. J. Roddy, R. O. Pepin, Academic, New York. and R. B. Merrill, eds.), pp. 639–656. Pergamon, New York. Adams J. B. and McCord T. B. (1973) Vitrification darkening Albee A. L. and Chodos A. A. (1970) Microprobe investigations in the lunar highlands and identification of Descartes on Apollo 11 samples. Proc. Apollo 11 Lunar Sci. Conf., pp. material at the Apollo 16 site. Proc. Lunar Sci. Conf. 4th, 135–157. pp. 163–177. Albee A. L., Chodos A. A., Gancarz A. J., Haines E. L., Adams J. B., Pieters C., and McCord T. B. (1974) Orange Papanastassiou D. A., Ray L., Tera F., Wasserburg G. J., glass: Evidence for regional deposits of pyroclastic origin and Wen T. (1972) Mineralogy, petrology, and chemistry of on the Moon.
    [Show full text]