Magnetotelluric Evidence for Layered Mafic Intrusions Beneath the VÃ
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Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
NINETY-NINE 9\Je\Ns
NINETY-NINE THE INTERNATIONAL WOMEN PILOT S MAGAZINE J _________ November-December,N 1993 • Crater Lake Flyers • !Ange(s — Corporate Angel Network • Becoming a “FED” Successful Board Meeting Reflects Fresh Outlook Just ask the Governors who were present; they didn’t pick up their knitting once - well, maybe once! The fall Board agenda was packed with items for discussion and action. On pages 10, 11 and 15 of this issue you’ll find detailed reports covering many of the items we evaluated, discussed, voted on, remanded for additional President’s Message information or to a committee, etc. We selected a new N e w s editor, Betty Rowley, and extended our thanks to Ann Cooper for her wonderful effort as editor. We discussed an informal proposal made by a member of the Atchison Historical Society Board that The 99s consider deeding 60 percent ownership of the Amelia Earhart Birthplace Museum to the Historical Society. In exchange, an undefined amount of funding for restoration would be made available. The Board unanimously decided they needed considerably more information Board members Alexis Koehler, Connie Woods, Joyce Wells, Gene Nora Jessen, Doris before an accurate assessment of this Abbate, Lee Orr, Carolyn Carpp, Lu Hollander and Lois Erickson pause during a full early-stage proposal could be fairly Board meeting schedule to look at one of the many early-day scrapbooks housed at 99s' International Headquarters. evaluated and acted upon. This addi tional information has been requested from the 99s’ Birthplace Museum Board, and will be available for further consideration prior to the spring Board meeting. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
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. -
Science Training History of the Apollo Astronauts William C
NASA/SP-2015-626 Science Training History of the Apollo Astronauts William C. Phinney National Aeronautics and Space Administration Apollo 17 crewmembers Gene Cernan and Harrison Schmitt conducting a practice EVA in the southern Nevada Volcanic Field near Tonopah, NV (NASA Photograph AS17-S72-48930). ii NASA/SP-2015-626 Science Training History of the Apollo Astronauts William C. Phinney National Aeronautics and Space Administration Cover photographs: From top: Apollo 13 Commander (CDR) James Lovell, left, and Lunar Module Pilot (LMP) Fred Haise during a geologic training trip to Kilbourne Hole, NM, November 1969 (NASA Photography S69- 25199); (Center) Apollo 16 LMP Charles Duke (left) and CDR John W. Young (right) during a practice EVA at Sudbury Crater, Ontario, Canada, July 1971 (NASA Photograph AS16-S71-39840); Apollo 17 LMP Harrison Schmitt (left) and CDR Eugene Cernan (right) during a practive EVA at Lunar Crater Volcanic Field, Tonopah, Nevada, September 1972 (NASA Photograph AS17-S72-48895); Apollo 15 CDR David Scott (left) and James Irwin (right) during practice geologic EVA training at the Rio Grande Gorge, Taos, NM, March 1971 (NASA Photograph AS15-S71-23773) iv ACKNOWLEDGEMENTS When I retired from NASA several of my coworkers, particularly Dave McKay and Everett Gibson, suggested that, given my past role as the coordinator for the science training of the Apollo astronauts, I should put together a history of what was involved in that training. Because it had been nearly twenty-five years since the end of Apollo they pointed out that many of the persons involved in that training might not be around when advice might be sought for future missions of this type. -
The Case for Rainfall on a Warm, Wet Early Mars Robert A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. E11, 5111, doi:10.1029/2001JE001505, 2002 The case for rainfall on a warm, wet early Mars Robert A. Craddock Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, District of Columbia, USA Alan D. Howard Department of Environmental Sciences, University of Virginia, Charlottesville, Virginia, USA Received 11 April 2001; revised 10 April 2002; accepted 10 June 2002; published 23 November 2002. [1] Valley networks provide compelling evidence that past geologic processes on Mars were different than those seen today. The generally accepted paradigm is that these features formed from groundwater circulation, which may have been driven by differential heating induced by magmatic intrusions, impact melt, or a higher primordial heat flux. Although such mechanisms may not require climatic conditions any different than today’s, they fail to explain the large amount of recharge necessary for maintaining valley network systems, the spatial patterns of erosion, or how water became initially situated in the Martian regolith. In addition, there are no clear surface manifestations of any geothermal systems (e.g., mineral deposits or phreatic explosion craters). Finally, these models do not explain the style and amount of crater degradation. To the contrary, analyses of degraded crater morphometry indicate modification occurred from creep induced by rain splash combined with surface runoff and erosion; the former process appears to have continued late into Martian history. A critical analysis of the morphology and drainage density of valley networks based on Mars Global Surveyor data shows that these features are, in fact, entirely consistent with rainfall and surface runoff. -
Sources of Extraterrestrial Rare Earth Elements: to the Moon and Beyond
resources Article Sources of Extraterrestrial Rare Earth Elements: To the Moon and Beyond Claire L. McLeod 1,* and Mark. P. S. Krekeler 2 1 Department of Geology and Environmental Earth Sciences, 203 Shideler Hall, Miami University, Oxford, OH 45056, USA 2 Department of Geology and Environmental Earth Science, Miami University-Hamilton, Hamilton, OH 45011, USA; [email protected] * Correspondence: [email protected]; Tel.: 513-529-9662; Fax: 513-529-1542 Received: 10 June 2017; Accepted: 18 August 2017; Published: 23 August 2017 Abstract: The resource budget of Earth is limited. Rare-earth elements (REEs) are used across the world by society on a daily basis yet several of these elements have <2500 years of reserves left, based on current demand, mining operations, and technologies. With an increasing population, exploration of potential extraterrestrial REE resources is inevitable, with the Earth’s Moon being a logical first target. Following lunar differentiation at ~4.50–4.45 Ga, a late-stage (after ~99% solidification) residual liquid enriched in Potassium (K), Rare-earth elements (REE), and Phosphorus (P), (or “KREEP”) formed. Today, the KREEP-rich region underlies the Oceanus Procellarum and Imbrium Basin region on the lunar near-side (the Procellarum KREEP Terrain, PKT) and has been tentatively estimated at preserving 2.2 × 108 km3 of KREEP-rich lithologies. The majority of lunar samples (Apollo, Luna, or meteoritic samples) contain REE-bearing minerals as trace phases, e.g., apatite and/or merrillite, with merrillite potentially contributing up to 3% of the PKT. Other lunar REE-bearing lunar phases include monazite, yittrobetafite (up to 94,500 ppm yttrium), and tranquillityite (up to 4.6 wt % yttrium, up to 0.25 wt % neodymium), however, lunar sample REE abundances are low compared to terrestrial ores. -
Copper Enrichments in the Kimberley Formation in Gale Crater, Mars
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Archive Ouverte en Sciences de l'Information et de la Communication Copper enrichments in the Kimberley formation in Gale crater, Mars: Evidence for a Cu deposit at the source Valérie Payré, Cécile Fabre, Violaine Sautter, Agnès Cousin, Nicolas Mangold, Laetitia Le Deit, Olivier Forni, Walter Goetz, Roger Wiens, Olivier Gasnault, et al. To cite this version: Valérie Payré, Cécile Fabre, Violaine Sautter, Agnès Cousin, Nicolas Mangold, et al.. Copper enrich- ments in the Kimberley formation in Gale crater, Mars: Evidence for a Cu deposit at the source. Icarus, Elsevier, 2019, 321, pp.736-751. 10.1016/j.icarus.2018.12.015. hal-02104588 HAL Id: hal-02104588 https://hal.archives-ouvertes.fr/hal-02104588 Submitted on 19 Apr 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. Accepted Manuscript Copper enrichments in the Kimberley formation in Gale crater, Mars: Evidence for a Cu deposit at the source Valerie« Payre« , Cecile« Fabre , Violaine Sautter , Agnes` Cousin , Nicolas Mangold , Laetitia Le Deit , Olivier Forni , Walter Goetz , Roger C. Wiens , Olivier Gasnault , Pierre-Yves Meslin , Jer« emie« Lasue , William Rapin , Ben Clark , Marion Nachon , Nina L. -
African Meteorite Impact Craters: Characteristics and Geological Importance
Journal of African Earth Sciences, Vol. 18, No. 4, pp. 263-295, 1994 Pergamon Copyright © 1994 Elsevier Science Ltd Printed in Great Britain. All rights reserved 0899-5362/94 $7.00 + 0.00 0899-5362(94)00044-1 African meteorite impact craters: characteristics and geological importance CHRISTIAN KOEBERLt~ 1Institute of Geochemistry, University of Vienna, Dr.-Karl-Lueger-Ring 1, A-1010 Vienna, Austria. 2Economic Geology Research Unit, Depa~ i.ment of Geology, University of the Witwatemmnd,Johannesburg 2050, South Africa. (Received 26 October 1993 : accepted 12 May 1994) Abslzact - Geologists have realized that impact cratering is the single most important surface-forming and modifying process for the other terrestrial planets and the satellites of all planets. The recognition of impact cratering as an important geological process on earth has been rather slow. However, geologists are now realizing that giant impacts have had a determining influence on the geological and biological evolution of our planet. The study of impact craters allows important conclusions, not only about the origin mid history of our solar system and its planets, but also about a fundamentally important geological process. In addition, impact craters may have a definite economic importance as some craters have been shown to contain important mineral or oil deposits. F'dtesn meteorite impact craters have so far been identified on the African continent:. Amguid (Algeria), Aomunga (Chad), Aouelloul (Mauritania), B.P. (Libya), Bosumtwi (Ghana), Highbury (Zimbabwe), Kalkkop (South Africa), Oasis (Libya), Ouarkziz (Algeria), Roter Kamm (Namibia), Saitpan (South Africa), Talemzane (Algeria), Tenoumer (Mauritania), T'm Bider (Algeria), and V~:lefort (South Africa). -
Planet Formation: Key Mechanisms and Global Models
Planet formation: key mechanisms and global models Sean N. Raymond and Alessandro Morbidelli Abstract Models of planet formation are built on underlying physical processes. In order to make sense of the origin of the planets we must first understand the origin of their building blocks. This review comes in two parts. The first part presents a detailed description of six key mechanisms of planet formation: • The structure and evolution of protoplanetary disks • The formation of planetesimals • Accretion of protoplanets • Orbital migration of growing planets • Gas accretion and giant planet migration • Resonance trapping during planet migration While this is not a comprehensive list, it includes processes for which our under- standing has changed in recent years or for which key uncertainties remain. The second part of this review shows how global models are built out of planet formation processes. We present global models to explain different populations of known planetary systems, including close-in small/low-mass planets (i.e., super- Earths), giant exoplanets, and the Solar System’s planets. We discuss the different sources of water on rocky exoplanets, and use cosmochemical measurements to constrain the origin of Earth’s water. We point out the successes and failings of different models and how they may be falsified. Finally, we lay out a path for the future trajectory of planet formation studies. Sean N. Raymond arXiv:2002.05756v1 [astro-ph.EP] 13 Feb 2020 Laboratoire d’Astrophysique de Bordeaux, CNRS and Université de Bordeaux, Pessac, France e-mail: [email protected] Alessandro Morbidelli Laboratoire Lagrange, Observatoire de la Cote d’Azur, Nice, France e-mail: [email protected] 1 2 Sean N. -
Toward a Conceptual Framework for Assessing the Human Dimensions of Paleontological Resources
Sullivan, R.M. and Lucas, S.G., eds., 2016, Fossil Record 5. New Mexico Museum of Natural History and Science Bulletin 74. 239 TOWARD A CONCEPTUAL FRAMEWORK FOR ASSESSING THE HUMAN DIMENSIONS OF PALEONTOLOGICAL RESOURCES VINCENT L. SANTUCCI¹, PETER NEWMAN² and B. DERRICK TAFF² 1National Park Service, 1201 Eye Street NW., Washington, D.C. 20005; -email: [email protected] 2The Pennsylvania State University, 801 Ford Building, University Park, PA 16802 Abstract—Dinosaurs and other fossils capture the imagination of people of all ages from around the globe. An assessment of the wide range of human values associated with paleontological resources reveals strong and sometimes conflicting perspectives. Given the fact that fossils are non-renewable resources, decision-making relative to the use, conservation and stewardship of paleontological resources must recognize and consider the human dimensions of fossils. Scientific, educational, recreational, commercial and other human values may directly influence the motivations and behaviors of individuals as they relate to paleontological resources. The unauthorized collection of fossils from public lands, including theft and vandalism, entails a variety of legal, ethical, economic and social factors that need to be assessed in conjunction with the planning and implementation of public policy. The purpose of this review is to initiate the compilation of baseline information on the human dimensions of paleontological resources in order to develop a conceptual framework and more clearly identify the most crucial questions to address in future research. INTRODUCTION and others to better understand and implement effective strategies for A fundamental topic in paleontology that has garnered little the enjoyment, use, management and stewardship of non-renewable attention is an evaluation of the values that humans ascribe to fossils. -
Science Concept 3: Key Planetary Processes Are Manifested in the Diversity of Lunar Crustal Rocks
Science Concept 3: Key Planetary Processes are Manifested in the Diversity of Lunar Crustal Rocks Science Concept 3: Key planetary processes are manifested in the diversity of crustal rocks Science Goals: a. Determine the extent and composition of the primary feldspathic crust, KREEP layer, and other products of differentiation. b. Inventory the variety, age, distribution, and origin of lunar rock types. c. Determine the composition of the lower crust and bulk Moon. d. Quantify the local and regional complexity of the current lunar crust. e. Determine the vertical extent and structure of the megaregolith. INTRODUCTION Formation and Evolution of the Moon The Moon is a unique environment, preserving crucial information about the early history and later evolution of the solar system. The lack of major surficial tectonic processes within the past few billion years or so, as well as the lack of significant quantities of surface water, have allowed for excellent preservation of the lithologies and geomorphological features that formed during the major planetary formation events. Fundamental discoveries during the Apollo program showed that the Moon is made up of a variety of volcanic and impact rock types that exhibit a particular range of chemical and mineralogical compositions. The key planetary processes conveyed by this diversity include planetary differentiation, volcanism, and impact cratering. Analysis of Apollo, Luna, and lunar meteoritic samples, as well as orbital data from a series of lunar exploration missions, generated geophysical models that strove to tell the story of the Moon. However, such models are restricted in the sense that they are based on information gathered from the samples that have so far been acquired.