GSA TODAY • 2000 Medalists, Awardees, P
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Lunar Impact Crater Identification and Age Estimation with Chang’E
ARTICLE https://doi.org/10.1038/s41467-020-20215-y OPEN Lunar impact crater identification and age estimation with Chang’E data by deep and transfer learning ✉ Chen Yang 1,2 , Haishi Zhao 3, Lorenzo Bruzzone4, Jon Atli Benediktsson 5, Yanchun Liang3, Bin Liu 2, ✉ ✉ Xingguo Zeng 2, Renchu Guan 3 , Chunlai Li 2 & Ziyuan Ouyang1,2 1234567890():,; Impact craters, which can be considered the lunar equivalent of fossils, are the most dominant lunar surface features and record the history of the Solar System. We address the problem of automatic crater detection and age estimation. From initially small numbers of recognized craters and dated craters, i.e., 7895 and 1411, respectively, we progressively identify new craters and estimate their ages with Chang’E data and stratigraphic information by transfer learning using deep neural networks. This results in the identification of 109,956 new craters, which is more than a dozen times greater than the initial number of recognized craters. The formation systems of 18,996 newly detected craters larger than 8 km are esti- mated. Here, a new lunar crater database for the mid- and low-latitude regions of the Moon is derived and distributed to the planetary community together with the related data analysis. 1 College of Earth Sciences, Jilin University, 130061 Changchun, China. 2 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China. 3 Key Laboratory of Symbol Computation and Knowledge Engineering of Ministry of Education, College of Computer Science and Technology, Jilin University, 130012 Changchun, China. 4 Department of Information Engineering and Computer ✉ Science, University of Trento, I-38122 Trento, Italy. -
Cross-References ASTEROID IMPACT Definition and Introduction History of Impact Cratering Studies
18 ASTEROID IMPACT Tedesco, E. F., Noah, P. V., Noah, M., and Price, S. D., 2002. The identification and confirmation of impact structures on supplemental IRAS minor planet survey. The Astronomical Earth were developed: (a) crater morphology, (b) geo- 123 – Journal, , 1056 1085. physical anomalies, (c) evidence for shock metamor- Tholen, D. J., and Barucci, M. A., 1989. Asteroid taxonomy. In Binzel, R. P., Gehrels, T., and Matthews, M. S. (eds.), phism, and (d) the presence of meteorites or geochemical Asteroids II. Tucson: University of Arizona Press, pp. 298–315. evidence for traces of the meteoritic projectile – of which Yeomans, D., and Baalke, R., 2009. Near Earth Object Program. only (c) and (d) can provide confirming evidence. Remote Available from World Wide Web: http://neo.jpl.nasa.gov/ sensing, including morphological observations, as well programs. as geophysical studies, cannot provide confirming evi- dence – which requires the study of actual rock samples. Cross-references Impacts influenced the geological and biological evolu- tion of our own planet; the best known example is the link Albedo between the 200-km-diameter Chicxulub impact structure Asteroid Impact Asteroid Impact Mitigation in Mexico and the Cretaceous-Tertiary boundary. Under- Asteroid Impact Prediction standing impact structures, their formation processes, Torino Scale and their consequences should be of interest not only to Earth and planetary scientists, but also to society in general. ASTEROID IMPACT History of impact cratering studies In the geological sciences, it has only recently been recog- Christian Koeberl nized how important the process of impact cratering is on Natural History Museum, Vienna, Austria a planetary scale. -
Timeline of Natural History
Timeline of natural history This timeline of natural history summarizes significant geological and Life timeline Ice Ages biological events from the formation of the 0 — Primates Quater nary Flowers ←Earliest apes Earth to the arrival of modern humans. P Birds h Mammals – Plants Dinosaurs Times are listed in millions of years, or Karo o a n ← Andean Tetrapoda megaanni (Ma). -50 0 — e Arthropods Molluscs r ←Cambrian explosion o ← Cryoge nian Ediacara biota – z ←Earliest animals o ←Earliest plants i Multicellular -1000 — c Contents life ←Sexual reproduction Dating of the Geologic record – P r The earliest Solar System -1500 — o t Precambrian Supereon – e r Eukaryotes Hadean Eon o -2000 — z o Archean Eon i Huron ian – c Eoarchean Era ←Oxygen crisis Paleoarchean Era -2500 — ←Atmospheric oxygen Mesoarchean Era – Photosynthesis Neoarchean Era Pong ola Proterozoic Eon -3000 — A r Paleoproterozoic Era c – h Siderian Period e a Rhyacian Period -3500 — n ←Earliest oxygen Orosirian Period Single-celled – life Statherian Period -4000 — ←Earliest life Mesoproterozoic Era H Calymmian Period a water – d e Ectasian Period a ←Earliest water Stenian Period -4500 — n ←Earth (−4540) (million years ago) Clickable Neoproterozoic Era ( Tonian Period Cryogenian Period Ediacaran Period Phanerozoic Eon Paleozoic Era Cambrian Period Ordovician Period Silurian Period Devonian Period Carboniferous Period Permian Period Mesozoic Era Triassic Period Jurassic Period Cretaceous Period Cenozoic Era Paleogene Period Neogene Period Quaternary Period Etymology of period names References See also External links Dating of the Geologic record The Geologic record is the strata (layers) of rock in the planet's crust and the science of geology is much concerned with the age and origin of all rocks to determine the history and formation of Earth and to understand the forces that have acted upon it. -
Exploring the Bombardment History of the Moon
EXPLORING THE BOMBARDMENT HISTORY OF THE MOON Community White Paper to the Planetary Decadal Survey, 2011-2020 September 15, 2009 Primary Author: William F. Bottke Center for Lunar Origin and Evolution (CLOE) NASA Lunar Science Institute at the Southwest Research Institute 1050 Walnut St., Suite 300 Boulder, CO 80302 Tel: (303) 546-6066 [email protected] Co-Authors/Endorsers: Carlton Allen (NASA JSC) Mahesh Anand (Open U., UK) Nadine Barlow (NAU) Donald Bogard (NASA JSC) Gwen Barnes (U. Idaho) Clark Chapman (SwRI) Barbara A. Cohen (NASA MSFC) Ian A. Crawford (Birkbeck College London, UK) Andrew Daga (U. North Dakota) Luke Dones (SwRI) Dean Eppler (NASA JSC) Vera Assis Fernandes (Berkeley Geochronlogy Center and U. Manchester) Bernard H. Foing (SMART-1, ESA RSSD; Dir., Int. Lunar Expl. Work. Group) Lisa R. Gaddis (US Geological Survey) 1 Jim N. Head (Raytheon) Fredrick P. Horz (LZ Technology/ESCG) Brad Jolliff (Washington U., St Louis) Christian Koeberl (U. Vienna, Austria) Michelle Kirchoff (SwRI) David Kring (LPI) Harold F. (Hal) Levison (SwRI) Simone Marchi (U. Padova, Italy) Charles Meyer (NASA JSC) David A. Minton (U. Arizona) Stephen J. Mojzsis (U. Colorado) Clive Neal (U. Notre Dame) Laurence E. Nyquist (NASA JSC) David Nesvorny (SWRI) Anne Peslier (NASA JSC) Noah Petro (GSFC) Carle Pieters (Brown U.) Jeff Plescia (Johns Hopkins U.) Mark Robinson (Arizona State U.) Greg Schmidt (NASA Lunar Science Institute, NASA Ames) Sen. Harrison H. Schmitt (Apollo 17 Astronaut; U. Wisconsin-Madison) John Spray (U. New Brunswick, Canada) Sarah Stewart-Mukhopadhyay (Harvard U.) Timothy Swindle (U. Arizona) Lawrence Taylor (U. Tennessee-Knoxville) Ross Taylor (Australian National U., Australia) Mark Wieczorek (Institut de Physique du Globe de Paris, France) Nicolle Zellner (Albion College) Maria Zuber (MIT) 2 The Moon is unique. -
Impact of the Coronavirus Pandemic (COVID-19) Lockdown on Mental Health and Well-Being in the United Arab Emirates
ORIGINAL RESEARCH published: 16 March 2021 doi: 10.3389/fpsyt.2021.633230 Impact of the Coronavirus Pandemic (COVID-19) Lockdown on Mental Health and Well-Being in the United Arab Emirates Leila Cheikh Ismail 1,2,3, Maysm N. Mohamad 4, Mo’ath F. Bataineh 5, Abir Ajab 1,3, Amina M. Al-Marzouqi 3,6, Amjad H. Jarrar 4, Dima O. Abu Jamous 3, Habiba I. Ali 4, Haleama Al Sabbah 7, Hayder Hasan 1,3, Lily Stojanovska 4,8, Mona Hashim 1,3, Reyad R. Shaker Obaid 1,3, Sheima T. Saleh 1,3, Tareq M. Osaili 1,3,9 and Ayesha S. Al Dhaheri 4* 1 Department of Clinical Nutrition and Dietetics, College of Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, 2 Nuffield Department of Women’s & Reproductive Health, University of Oxford, Oxford, United Kingdom, 3 Research Institute of Medical and Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, 4 Department of Edited by: Nutrition and Health, College of Medicine and Health Sciences, United Arab Emirates University, Al Ain, United Arab Daniel Bressington, Emirates, 5 Department of Sport Rehabilitation, Faculty of Physical Education and Sport Sciences, The Hashemite University, Charles Darwin University, Australia Zarqa, Jordan, 6 Department of Health Services Administration, College of Health Sciences, Research Institute for Medical 7 Reviewed by: and Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, College of Natural and Health Sciences, Zayed University, Dubai, United Arab Emirates, 8 Institute for Health and Sport, Victoria University, Melbourne, VIC, Australia, Gianluca Serafini, 9 Department of Nutrition and Food Technology, Faculty of Agriculture, Jordan University of Science and Technology, San Martino Hospital (IRCCS), Italy Irbid, Jordan Andrea Aguglia, University of Genoa, Italy Andrea Amerio, United Arab Emirates (UAE) has taken unprecedented precautionary measures including University of Genoa, Italy complete lockdowns against COVID-19 to control its spread and ensure the well-being *Correspondence: Ayesha S. -
Asteroid Impact, Not Volcanism, Caused the End-Cretaceous Dinosaur Extinction
Asteroid impact, not volcanism, caused the end-Cretaceous dinosaur extinction Alfio Alessandro Chiarenzaa,b,1,2, Alexander Farnsworthc,1, Philip D. Mannionb, Daniel J. Luntc, Paul J. Valdesc, Joanna V. Morgana, and Peter A. Allisona aDepartment of Earth Science and Engineering, Imperial College London, South Kensington, SW7 2AZ London, United Kingdom; bDepartment of Earth Sciences, University College London, WC1E 6BT London, United Kingdom; and cSchool of Geographical Sciences, University of Bristol, BS8 1TH Bristol, United Kingdom Edited by Nils Chr. Stenseth, University of Oslo, Oslo, Norway, and approved May 21, 2020 (received for review April 1, 2020) The Cretaceous/Paleogene mass extinction, 66 Ma, included the (17). However, the timing and size of each eruptive event are demise of non-avian dinosaurs. Intense debate has focused on the highly contentious in relation to the mass extinction event (8–10). relative roles of Deccan volcanism and the Chicxulub asteroid im- An asteroid, ∼10 km in diameter, impacted at Chicxulub, in pact as kill mechanisms for this event. Here, we combine fossil- the present-day Gulf of Mexico, 66 Ma (4, 18, 19), leaving a crater occurrence data with paleoclimate and habitat suitability models ∼180 to 200 km in diameter (Fig. 1A). This impactor struck car- to evaluate dinosaur habitability in the wake of various asteroid bonate and sulfate-rich sediments, leading to the ejection and impact and Deccan volcanism scenarios. Asteroid impact models global dispersal of large quantities of dust, ash, sulfur, and other generate a prolonged cold winter that suppresses potential global aerosols into the atmosphere (4, 18–20). These atmospheric dinosaur habitats. -
Rare Earth Elements in Planetary Crusts: Insights from Chemically Evolved Igneous Suites on Earth and the Moon
minerals Article Rare Earth Elements in Planetary Crusts: Insights from Chemically Evolved Igneous Suites on Earth and the Moon Claire L. McLeod 1,* and Barry J. Shaulis 2 1 Department of Geology and Environmental Earth Sciences, 203 Shideler Hall, Miami University, Oxford, OH 45056, USA 2 Department of Geosciences, Trace Element and Radiogenic Isotope Lab (TRaIL), University of Arkansas, Fayetteville, AR 72701, USA; [email protected] * Correspondence: [email protected]; Tel.: +1-513-529-9662 Received: 5 July 2018; Accepted: 8 October 2018; Published: 16 October 2018 Abstract: The abundance of the rare earth elements (REEs) in Earth’s crust has become the intense focus of study in recent years due to the increasing societal demand for REEs, their increasing utilization in modern-day technology, and the geopolitics associated with their global distribution. Within the context of chemically evolved igneous suites, 122 REE deposits have been identified as being associated with intrusive dike, granitic pegmatites, carbonatites, and alkaline igneous rocks, including A-type granites and undersaturated rocks. These REE resource minerals are not unlimited and with a 5–10% growth in global demand for REEs per annum, consideration of other potential REE sources and their geological and chemical associations is warranted. The Earth’s moon is a planetary object that underwent silicate-metal differentiation early during its history. Following ~99% solidification of a primordial lunar magma ocean, residual liquids were enriched in potassium, REE, and phosphorus (KREEP). While this reservoir has not been directly sampled, its chemical signature has been identified in several lunar lithologies and the Procellarum KREEP Terrane (PKT) on the lunar nearside has an estimated volume of KREEP-rich lithologies at depth of 2.2 × 108 km3. -
NASA's Planetary Defense Coordination Office
National Aeronautics and Space Administration NASA’s Planetary Defense Coordination Office NASA Infrared Near-Earth Pan-STARRS Comet ISON Goldstone Radar Near-Earth Telescope Facility Asteroid Eros Observatory Asteroid Bennu www.nasa.gov What are near-Earth objects and why do we need sanctioned by the International Astronomical Union What is NASA doing to prepare for planetary to study them? and supported by the NEO Observations Program. defense? Near-Earth objects (NEOs) are asteroids and comets NASA-funded surveys have found 98 percent of the NASA has a Planetary Defense Coordination Office that have been nudged by the gravitational attraction known catalog of over 20,000 near-Earth objects (only (PDCO) located at NASA Headquarters in Washington, of nearby planets into orbits that allow them to enter a little more than 100 of these objects are comets). D.C. Its responsibilities include: Earth’s neighborhood. Like the planets, all asteroids These surveys are currently finding NEOs at a rate of • Ensuring the early detection of potentially hazardous and comets orbit the Sun. They are remnants of the about 1,800 per year. The current objective of the NEO objects (PHOs) – asteroids and comets whose orbits formation of planetary bodies in our solar system. Observations Program is to find, track, and catalog at are predicted to bring them within 5 million miles least 90 percent of the estimated population of NEOs (8 million kilometers) of Earth; and of a size large Our solar system contains far more asteroids than that are equal to or greater than 140 meters in size in enough to reach Earth’s surface – that is, greater comets, and thus far more near-Earth asteroids than coming years and to characterize a subset of those than around 30 to 50 meters; near-Earth comets. -
The End-Cretaceous Mass Extinction Event at the Impact Area: a Rapid Macrobenthic Diversification and Stabilization
EPSC Abstracts Vol. 14, EPSC2020-65, 2020 https://doi.org/10.5194/epsc2020-65 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. The end-Cretaceous mass extinction event at the impact area: A rapid macrobenthic diversification and stabilization Francisco Javier Rodriguez Tovar1, Christopher M. Lowery2, Timothy J. Bralower3, Sean P.S. Gulick2,4,5, and Heather L. Jones3 1University of Granada, Stratigraphy and Palaeontology, Granada, Spain ([email protected]) 2Institute for Geophysics, Jackson School of Geosciences, University of Texas at Austin, Austin, Texas 78758, USA 3Department of Geosciences, Pennsylvania State University, University Park, Pennsylvania 16802, USA 4Center for Planetary Systems Habitability, University of Texas at Austin, Austin, Texas 11 78712, USA 5Department of Geological Sciences, Jackson School of Geosciences, University of Texas at Austin, Austin, Texas 78712, USA The Cretaceous-Paleogene (K-Pg) mass extinction, 66.0 Ma (Renne et al., 2013), was one of the most important events in the Phanerozoic, severely altering the evolutionary and ecological history of biotas (Schulte et al., 2010). This extinction was caused by paleoenvironmental changes associated with the impact of an asteroid (Alvarez et al., 1980) on the Yucatán carbonate-evaporite platform in the southern Gulf of Mexico, which formed the Chicxulub impact crater (Hildebrand et al., 1991). Prolonged impact winter resulting in global darkness and cessation of photosynthesis, and acid rain have been considered as major killing mechanisms on land and in the oceans. Major animal groups disappeared across the boundary (e.g., the nonavian dinosaurs, marine and flying reptiles, ammonites, and rudists), and other groups suffered severe species level (but not total) extinction, including planktic foraminifera, and calcareous nannofossils. -
Children and Disasters: Understanding Impact and Enabling Agency Fran Seballos, Thomas Tanner, Marcela Tarazona and Jose Gallegos
Research Report Children and Disasters: Understanding Impact and Enabling Agency Fran Seballos, Thomas Tanner, Marcela Tarazona and Jose Gallegos May 2011 1 Children and Disasters: Understanding Impact and Enabling Agency Acknowledgements Photos: The research and production of this report was funded by partners of the Children in a Changing Climate (CCC) coalition: UNICEF, World Vision International, Plan • Front cover top – A woman and International and Save the Children International with additional funds from UNISDR. child watch the flood water rise from The Institute of Development Studies led the writing and production of the synthesis the door of their makeshift home report; thanks go in particular to Lucy Stone of UNICEF UK for her inputs. in Kamrangir Char, Dhaka, 2004 www.childreninachangingclimate.org (Photo: Naser Siddique, UNICEF). Data analysis was led by Oxford Policy Management. Particular thanks go to staff at Bottom – Children present their DRR UNICEF Geneva and the UNICEF Country Offices in Bolivia, Mexico, Mozambique, work to the community, El Matazano, Nepal, Vietnam, Indonesia, and the Philippines who sourced and collated socio- El Salvador 2009 (Photo: T. Tanner,) economic data sets and to staff at UNISDR who provided ongoing support regarding the Desinventar disaster dataset. Their expertise and enthusiasm were invaluable. • Above – Children mix cement to build a retaining wall at their school, The enabling environments research draws on an Institute of Development Studies Potrerillos, El Salvador 2010 (Photo: (IDS) research programme funded by the UK Economic and Social Research Council T. Tanner) (ESRC, grant no. RES-061-25-0148) and Plan UK, and was supplemented by additional research for this report. -
Persistence and Origin of the Lunar Core Dynamo
Persistence and origin of the lunar core dynamo Clément Suaveta,1, Benjamin P. Weissa, William S. Cassatab, David L. Shusterc,d, Jérôme Gattaccecaa,e, Lindsey Chanf, Ian Garrick-Bethellf,g, James W. Headh, Timothy L. Grovea, and Michael D. Fulleri aDepartment of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139; bChemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550; cDepartment of Earth and Planetary Science, University of California, Berkeley, CA 94720; dBerkeley Geochronology Center, Berkeley, CA 94709; eCentre Européen de Recherche et d’Enseignement des Géosciences de l’Environnement, Centre National de la Recherche Scientifique, Université Aix-Marseille 3, 13545 Aix-en-Provence, France; fDepartment of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064; gSchool of Space Research, Kyung Hee University, Yongin 446–701, South Korea; hDepartment of Geological Sciences, Brown University, Providence, RI 02912; and iHawai’i Institute of Geophysics and Planetology, University of Hawaii at Manoa, Honolulu, HI 96822 Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved April 16, 2013 (received for review January 22, 2013) The lifetime of the ancient lunar core dynamo has implications for its 10017 as a constraint on the lunar dynamo. Instead, these authors power source and the mechanism of field generation. Here, we report relied on their analyses of 10049, whose subsamples were found to analyses of two 3.56-Gy-old mare basalts demonstrating that they carry a unidirectional magnetization (17) with a seemingly weak were magnetized in a stable and surprisingly intense dynamo mag- paleointensity (4–10 μT). However, our reanalysis of their data netic field of at least ∼13 μT. -
Hadean-Archean Habitability
Hadean - Early Archean: 4.4 to ~ 3.5 Ga How to build a habitable planet? Jack Hills in Australia meta-conglomerat with the oldest minerals on Earth 4.4 Ga Geological time scale 1 : Hadean 2 : Archean Quasi no rock record Rock record First cooling of magma ocean Alteration of basalt to produce serpentinite crust ~ as today on seafloor 146 142 Sm → Nd (T1/2= 103 Ma) silicate/silicate fractionation before total decay of 146Sm ⇒ < 150 Ma, done early Hadean Acasta (Canada) oldest rocks on Earth, end of Hadean, 4.01 Ga Acasta (Canada) oldest rocks on Earth, end of Hadean, 4.01 Ga Acasta (Canada) oldest rocks on Earth, end of Hadean, 4.01 Ga Zircon ages Jack Hills (Australia) meta-conglomerat Archean in age but contains very old zircons Jack Hills (Australia) meta-conglomerat Archean in age but contains very old zircons Jack Hills (Australia) meta-conglomerat Archean in age but contains very old zircons ZrSiO4 1 mm U-Pb age at 4.4 Ga Part of the grain crystalized shortly after end of magma ocean Age distribution of zircons Different dates on different zircon layers Several age populations Oldest Quartz, micas and plagioclase ∂18O in zircons = 5 to 7.4 ‰ Original magma’s = ∂18O ~ 8.5 to 9.5‰ (La/Lu)N zircons⇒(La/Lu)N of magma~ 200 = TTG magma 4.4 Gyr zircons not so different from actual zircons Granitic inclusions present in zircons Quartz, micas and plagioclase ∂18O in zircons = 5 to 7.4 ‰ Original magma’s = ∂18O ~ 8.5 to 9.5‰ (La/Lu)N zircons⇒(La/Lu)N of magma~ 200 = TTG magma 4.4 Gyr zircons not so different from actual zircons Continental