Earth Science Literacy Principles
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Preprint Arxiv:1806.10939, 2018
Solid Earth Discuss., https://doi.org/10.5194/se-2019-4 Manuscript under review for journal Solid Earth Discussion started: 15 January 2019 c Author(s) 2019. CC BY 4.0 License. Bayesian geological and geophysical data fusion for the construction and uncertainty quantification of 3D geological models Hugo K. H. Olierook1, Richard Scalzo2, David Kohn3, Rohitash Chandra2,4, Ehsan Farahbakhsh2,4, Gregory Houseman3, Chris Clark1, Steven M. Reddy1, R. Dietmar Müller4 5 1School of Earth and Planetary Sciences, Curtin University, GPO Box U1987, Perth, WA 6845, Australia 2Centre for Translational Data Science, University of Sydney, NSW 2006 Sydney, Australia 3Sydney Informatics Hub, University of Sydney, NSW 2006 Sydney, Australia 4EarthByte Group, School of Geosciences, University of Sydney, NSW 2006 Sydney, Australia Correspondence to: Hugo K. H. Olierook ([email protected]) 10 Abstract. Traditional approaches to develop 3D geological models employ a mix of quantitative and qualitative scientific techniques, which do not fully provide quantification of uncertainty in the constructed models and fail to optimally weight geological field observations against constraints from geophysical data. Here, we demonstrate a Bayesian methodology to fuse geological field observations with aeromagnetic and gravity data to build robust 3D models in a 13.5 × 13.5 km region of the Gascoyne Province, Western Australia. Our approach is validated by comparing model results to independently-constrained 15 geological maps and cross-sections produced by the Geological Survey of Western Australia. By fusing geological field data with magnetics and gravity surveys, we show that at 89% of the modelled region has >95% certainty. The boundaries between geological units are characterized by narrow regions with <95% certainty, which are typically 400–1000 m wide at the Earth’s surface and 500–2000 m wide at depth. -
Callisto: a Guide to the Origin of the Jupiter System
A PAPER SUBMITTED TO THE DECADAL SURVEY ON PLANETARY SCIENCE AND ASTROBIOLOGY Callisto: A Guide to the Origin of the Jupiter System David E Smith 617-803-3377 Department of Earth, Atmospheric and PLanetary Sciences Massachusetts Institute of Technology, Cambridge MA 02139 [email protected] Co-authors: Francis Nimmo, UCSC, [email protected] Krishan Khurana, UCLA, [email protected] Catherine L. Johnson, PSI, [email protected] Mark Wieczorek, OCA, Fr, [email protected] Maria T. Zuber, MIT, [email protected] Carol Paty, University of Oregon, [email protected] Antonio Genova, Univ Rome, It, [email protected] Erwan Mazarico, NASA GSFC, [email protected] Louise Prockter, LPI, [email protected] Gregory A. Neumann, NASA GSFC Emeritus, [email protected] John E. Connerney, Adnet Systems Inc., [email protected] Edward B. Bierhaus, LMCO, [email protected] Sander J. Goossens, UMBC, [email protected] MichaeL K. Barker, NASA GSFC, [email protected] Peter B. James, Baylor, [email protected] James Head, Brown, [email protected] Jason Soderblom, MIT, [email protected] July 14, 2020 Introduction Among the GaLiLean moons of Jupiter, it is outermost CaLListo that appears to most fulLy preserve the record of its ancient past. With a surface aLmost devoid of signs of internaL geologic activity, and hints from spacecraft data that its interior has an ocean whiLe being only partiaLLy differentiated, CaLListo is the most paradoxicaL of the giant rock-ice worlds. How can a body with such a primordiaL surface harbor an ocean? If the interior was warm enough to form an ocean, how could a mixed rock and ice interior remain stable? What do the striking differences between geologicaLLy unmodified CaLListo and its sibling moon Ganymede teLL us about the formation of the GaLiLean moons and the primordiaL conditions at the time of the formation of CaLListo and the accretion of giant planet systems? The answers can be provided by a CaLListo orbitaL mission. -
The History of Planet Earth
SECOND EDITION Earth’s Evolving The History of Systems Planet Earth Ronald Martin, Ph.D. University of Delaware Newark, Delaware © Jones & Bartlett Learning, LLC, an Ascend Learning Company. NOT FOR SALE OR DISTRIBUTION 9781284457162_FMxx_00i_xxii.indd 1 07/11/16 1:46 pm World Headquarters Jones & Bartlett Learning 5 Wall Street Burlington, MA 01803 978-443-5000 [email protected] www.jblearning.com Jones & Bartlett Learning books and products are available through most bookstores and online booksellers. To contact Jones & Bartlett Learning directly, call 800-832-0034, fax 978-443-8000, or visit our website, www.jblearning.com. Substantial discounts on bulk quantities of Jones & Bartlett Learning publications are available to corporations, professional associations, and other qualified organizations. For details and specific discount information, contact the special sales department at Jones & Bartlett Learning via the above contact information or send an email to [email protected]. Copyright © 2018 by Jones & Bartlett Learning, LLC, an Ascend Learning Company All rights reserved. No part of the material protected by this copyright may be reproduced or utilized in any form, electronic or mechanical, including photocopying, recording, or by any information storage and retrieval system, without written permission from the copyright owner. The content, statements, views, and opinions herein are the sole expression of the respective authors and not that of Jones & Bartlett Learning, LLC. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement or recommendation by Jones & Bartlett Learning, LLC, and such reference shall not be used for advertis- ing or product endorsement purposes. -
Nature Based Solutions FEMA
PROMOTING NATURE-BASED HAZARD MITIGATION THROUGH FEMA MITIGATION GRANTS ABBREVIATIONS ADCIRC – Advanced Circulation Model HGM Approach – Hydrogeomorphic Approach BCA – Benefit-Cost Analysis HMA – Hazard Mitigation Assistance BCR – Benefit-Cost Ratio HMGP – Hazard Mitigation Grant Program BRIC – Building Resilient Infrastructure and MSCP – Multiple Species Conservation Program Communities NBS – Nature-Based Solution C&CB – Capability- and Capacity-Building NFIP – National Flood Insurance Program CDBG-DR – Community Development Block Grant- Disaster Recovery NFWF – National Fish and Wildlife Foundation CDBG-MIT – Community Development Block NOAA – National Oceanic and Atmospheric Grant-Mitigation Administration D.C. – District of Columbia NOFO – Notice of Funding Opportunity DEM – Department of Emergency Management NPV – Net Present Value DOI – Department of the Interior SCC – State Coastal Conservancy EDYS – Ecological Dynamics Simulation SDG&E – San Diego Gas & Electric EMA – Emergency Management Agency SFHA – Special Flood Hazard Area EPA SWMM – Environmental Protection Agency SHMO – State Hazard Mitigation Officer Storm Water Management Model SLAMM – Sea Level Affecting Marshes Model FEMA – Federal Emergency Management Agency SRH-2D – Sedimentation and River Hydraulics – FIRM – Flood Insurance Rate Map Two-Dimension FMA – Flood Mitigation Assistance STWAVE – Steady-State Spectral Wave Model FMAG – Fire Management Assistance Grant TNC – The Nature Conservancy HAZUS – Hazards US USACE – U.S. Army Corps of Engineers HEC-HMS – Hydrologic -
Dwarf Planet Ceres
Dwarf Planet Ceres drishtiias.com/printpdf/dwarf-planet-ceres Why in News As per the data collected by NASA’s Dawn spacecraft, dwarf planet Ceres reportedly has salty water underground. Dawn (2007-18) was a mission to the two most massive bodies in the main asteroid belt - Vesta and Ceres. Key Points 1/3 Latest Findings: The scientists have given Ceres the status of an “ocean world” as it has a big reservoir of salty water underneath its frigid surface. This has led to an increased interest of scientists that the dwarf planet was maybe habitable or has the potential to be. Ocean Worlds is a term for ‘Water in the Solar System and Beyond’. The salty water originated in a brine reservoir spread hundreds of miles and about 40 km beneath the surface of the Ceres. Further, there is an evidence that Ceres remains geologically active with cryovolcanism - volcanoes oozing icy material. Instead of molten rock, cryovolcanoes or salty-mud volcanoes release frigid, salty water sometimes mixed with mud. Subsurface Oceans on other Celestial Bodies: Jupiter’s moon Europa, Saturn’s moon Enceladus, Neptune’s moon Triton, and the dwarf planet Pluto. This provides scientists a means to understand the history of the solar system. Ceres: It is the largest object in the asteroid belt between Mars and Jupiter. It was the first member of the asteroid belt to be discovered when Giuseppe Piazzi spotted it in 1801. It is the only dwarf planet located in the inner solar system (includes planets Mercury, Venus, Earth and Mars). Scientists classified it as a dwarf planet in 2006. -
Amplify Science Earth's Changing Climate
Lawrence Hall of Science has new instructional materials that address the Next Generation Science Standards! Check out these Middle School Units… As just one example, compare Middle School units from three different Hall programs. See for yourself how each program goes about addressing the Middle School NGSS Standards related to Human Impacts and Climate Change, and choose the approach that best meets the needs of your school district. MS NGSS Performance Expectations: Human Impacts and Climate Change • MS-ESS3-2. Analyze and interpret data on natural hazards to forecast future catastrophic events and inform the development of technologies to mitigate their effects. • MS-ESS3-3. Apply scientific principles to design a method for monitoring and minimizing a human impact on the Environment. • MS-ESS3-4. Construct an argument supported by evidence for how increases in human population and per-capita consumption of natural resources impact Earth’s systems. • MS-ESS3-5. Ask questions to clarify evidence of the factors that have caused the rise in global temperatures over the past century. Sample Units from Three Different Hall Programs • Amplify Science—Earth’s Changing Climate: Vanishing Ice Earth’s Changing Climate Engineering Internship • FOSS—Weather and Water • Ocean Sciences Sequence—The Ocean-Atmosphere Connection and Climate Change ©The Regents of the University of California ©The Regents of the University of California Description of two Middle School units from Amplify Science Earth’s Changing Climate: Vanishing Ice and Earth’s Changing Climate Engineering Internship Grade 6-8 Units — requiring at least 19 and 10 45-minute class sessions respectively (two of 27 Middle School Amplify Science units) The Problem: Why is the ice on Earth’s surface melting? Students’ Role: In the role of student climatologists, students investigate what is causing ice on Earth’s surface to melt in order to help the fictional World Climate Institute educate the public about the processes involved. -
Planets of the Solar System
Chapter Planets of the 27 Solar System Chapter OutlineOutline 1 ● Formation of the Solar System The Nebular Hypothesis Formation of the Planets Formation of Solid Earth Formation of Earth’s Atmosphere Formation of Earth’s Oceans 2 ● Models of the Solar System Early Models Kepler’s Laws Newton’s Explanation of Kepler’s Laws 3 ● The Inner Planets Mercury Venus Earth Mars 4 ● The Outer Planets Gas Giants Jupiter Saturn Uranus Neptune Objects Beyond Neptune Why It Matters Exoplanets UnderstandingU d t di theth formationf ti and the characteristics of our solar system and its planets can help scientists plan missions to study planets and solar systems around other stars in the universe. 746 Chapter 27 hhq10sena_psscho.inddq10sena_psscho.indd 774646 PDF 88/15/08/15/08 88:43:46:43:46 AAMM Inquiry Lab Planetary Distances 20 min Turn to Appendix E and find the table entitled Question to Get You Started “Solar System Data.” Use the data from the How would the distance of a planet from the sun “semimajor axis” row of planetary distances to affect the time it takes for the planet to complete devise an appropriate scale to model the distances one orbit? between planets. Then find an indoor or outdoor space that will accommodate the farthest distance. Mark some index cards with the name of each planet, use a measuring tape to measure the distances according to your scale, and place each index card at its correct location. 747 hhq10sena_psscho.inddq10sena_psscho.indd 774747 22/26/09/26/09 111:42:301:42:30 AAMM These reading tools will help you learn the material in this chapter. -
The Solar System
5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5. -
THE PENNY MOON and QUARTER EARTH School Adapted from a Physics Forum Activity At
~ LPI EDUCATION/PUBLIC OUTREACH SCIENCE ACTIVITIES ~ Ages: 5th grade – high THE PENNY MOON AND QUARTER EARTH school Adapted from a Physics Forum activity at: http://www.phvsicsforums.com/ Duration: 10 minutes OVERVIEW — The students will use a penny and a quarter to model the Moon’s rotation on its axis and Materials: revolution around the Earth, and demonstrate that the Moon keeps the same face toward One penny and one the Earth. quarter per pair of students OBJECTIVE — Overhead projector, or The students will: elmo, or video Demonstrate the motion of the Moon’s rotation and revolution. projector Compare what we would see of the Moon if it did not rotate to what we see when its period of rotation is the same as its orbital period. Projected image of student overhead BEFORE YOU START: Do not introduce this topic along with the reason for lunar phases; students may become confused and assume that the Moon’s rotation is related to its phases. Prepare to show the student overhead projected for the class to see. ACTIVITY — 1. Ask your students to describe which parts of the Moon they see. Does the Moon turn? Can we see its far side? Allow time for your students to discuss this and share their opinions. 2. Hand out the pennies and quarters so that each pair of students has both. Tell the students that they will be creating a model of the Earth and Moon. Which object is Earth? [the quarter] Which one is the Moon? [the penny] 3. Turn on the projected student overhead. -
Geodynamics If the Entire Solid Earth Is Viewed As a Single Dynamic
http://www.paper.edu.cn Geodynamic Processes and Our Living Environment YANG Wencai, P. Robinson, FU Rongshan and WANG Ying Geological Publishing House: 2001 Geophysical System Yang Wencai, Institute of Geology, CAGS, China Key words: Geophysics, geodynamics, kinetics of the Earth, tectonics, energies of the Earth, driving forces, applied geophysics, sustainable development. Contents: I. About geophysical system II. Kinetics of the Earth III. About plate tectonics and plume tectonics IV. The contents in the topic V. Energies for the dynamic Earth VI. Driving Forces of Plate Tectonics VII. Geophysics and sustainable development of the society I. About geophysical system Rapid advance of sciences during the second half of the twentieth century has enabled man to make a successful star in the exploration of planetary space. The deep interior of the Earth, however, remains as inaccessible as ever. This is the realm of solid-Earth geophysics, which still mainly depends on observations made at or near the Earth's surface. Despite this limitation, a major revolution in knowledge of the Earth's interior has taken place over the last forty years. This has led to a new understanding of the processes which occur within the Earth that produce surface conditions outstandingly different from those of the other inner planets and the moon. How has this come about? It is mainly the results of the introduction of new experimental and computational techniques into geophysics. Geophysics as a major branch of the geosciences has been discussed in Topic 6.16.1. Theoretically and traditionally the geophysical system correlates to physical system, but specified st study the solid Earth, containing sub-branches such as gravitation and Earth-motion correlated with 转载 1 中国科技论文在线 http://www.paper.edu.cn mechanics, geothermics correlated with heat and thermics, seismology with acoustics and wave theory, geoelectricity and geomagnetism. -
Earth Science SCIH 041 055 Credits: 0.5 Units / 5 Hours / NCAA
UNIVERSITY OF NEBRASKA HIGH SCHOOL Earth Science SCIH 041 055 Credits: 0.5 units / 5 hours / NCAA Course Description Have you ever wondered where marble comes from? or how deep the ocean is? or why it rains more in areas near the Equator than in other places? In this course students will study a variety of topics designed to give them a better understanding of the planet on which we live. They will study the composition of Earth including minerals and different rock types, weathering and erosion processes, mass movements, and surface and groundwater. They will also explore Earth's atmosphere and oceans, including storms, climate and ocean movements, plate tectonics, volcanism, earthquakes, mountain building, and geologic time. This course concludes with an in-depth look at the connections between our Earth's vast resources and the human population's dependence and impact on them. Graded Assessments: 5 Unit Evaluations; 2 Projects; 2 Proctored Progress Tests, 5 Teacher Connect Activities Course Objectives When you have completed the materials in this course, you should be able to: 1. Describe how Earth materials move through geochemical cycles (carbon, nitrogen, oxygen) resulting in chemical and physical changes in matter. 2. Understand the relationships among Earth’s structure, systems, and processes. 3. Describe how heat convection in the mantle propels the plates comprising Earth’s surface across the face of the globe (plate tectonics). 4. Evaluate the impact of human activity and natural causes on Earth’s resources (groundwater, rivers, land, fossil fuels). 5. Describe the relationships among the sources of energy and their effects on Earth’s systems. -
Download Student Activities Objects from the Area Around Its Orbit, Called Its Orbital Zone; at Amnh.Org/Worlds-Beyond-Earth-Educators
INSIDE Essential Questions Synopsis Missions Come Prepared Checklist Correlation to Standards Connections to Other Halls Glossary ONLINE Student Activities Additional Resources amnh.org/worlds-beyond-earth-educators EssentialEssential Questions Questions What is the solar system? In the 20th century, humans began leaving Earth. NASA’s Our solar system consists of our star—the Sun—and all the Apollo space program was the first to land humans on billions of objects that orbit it. These objects, which are bound another world, carrying 12 human astronauts to the Moon’s to the Sun by gravity, include the eight planets—Mercury, surface. Since then we’ve sent our proxies—robots—on Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune; missions near and far across our solar system. Flyby several dwarf planets, including Ceres and Pluto; hundreds missions allow limited glimpses; orbiters survey surfaces; of moons orbiting the planets and other bodies, including landers get a close-up understanding of their landing Jupiter’s four major moons and Saturn’s seven, and, of course, location; and rovers, like human explorers, set off across the Earth’s own moon, the Moon; thousands of comets; millions surface to see what they can find and analyze. of asteroids; and billions of icy objects beyond Neptune. The solar system is shaped like a gigantic disk with the Sun at The results of these explorations are often surprising. With its center. Everywhere we look throughout the universe we the Moon as our only reference, we expected other worlds see similar disk-shaped systems bound together by gravity. to be cold, dry, dead places, but exploration has revealed Examples include faraway galaxies, planetary systems astonishing variety in our solar system.