The Lathrop Wells Volcanic Center: Status of Field and Geochronology
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9Th Grade Ela
9TH GRADE ELA Week of: MAY 11TH WICHITA PUBLIC SCHOOLS 9th, 10th, 11th and 12th Grades Your child should spend up to 90 minutes over the course of each day on this packet. Consider other family-friendly activities during the day such as: Learn how to do laundry. Create a cartoon image Make a bucket list of Look up riddles to Wash the laundry, of your family. things to do after the solve with someone fold and put the quarantine is over with in your family. laundry away. your family. Mindful Minute: Write Do a random act of Teach someone in your Put together a puzzle down what a typical day kindness for someone in family to play one of your with your family. was like pre-quarantine your house. video games. and during quarantine. How have things changed? *All activities are optional. Parents/Guardians please practice responsibility, safety, and supervision. For students with an Individualized Education Program (IEP) who need additional support, Parents/Guardians can refer to the Specialized Instruction and Supports webpage, contact their child’s IEP manager, and/or speak to the special education provider when you are contacted by them. Contact the IEP manager by emailing them directly or by contacting the school. The Specialized Instruction and Supports webpage can be accessed by clicking HERE or by navigating in a web browser to https://www.usd259.org/Page/17540 WICHITA PUBLIC SCHOOLS CONTINUOUS LEARNING HOTLINE AVAILABLE 316-973-4443 MARCH 30 – MAY 21, 2020 MONDAY – FRIDAY 11:00 AM – 1:00 PM ONLY For Multilingual Education Services (MES) support, please call (316) 866-8000 (Spanish and Proprio) or (316) 866-8003 (Vietnamese). -
Source to Surface Model of Monogenetic Volcanism: a Critical Review
Downloaded from http://sp.lyellcollection.org/ by guest on September 28, 2021 Source to surface model of monogenetic volcanism: a critical review I. E. M. SMITH1 &K.NE´ METH2* 1School of Environment, University of Auckland, Auckland, New Zealand 2Volcanic Risk Solutions, Massey University, Palmerston North 4442, New Zealand *Correspondence: [email protected] Abstract: Small-scale volcanic systems are the most widespread type of volcanism on Earth and occur in all of the main tectonic settings. Most commonly, these systems erupt basaltic magmas within a wide compositional range from strongly silica undersaturated to saturated and oversatu- rated; less commonly, the spectrum includes more siliceous compositions. Small-scale volcanic systems are commonly monogenetic in the sense that they are represented at the Earth’s surface by fields of small volcanoes, each the product of a temporally restricted eruption of a composition- ally distinct batch of magma, and this is in contrast to polygenetic systems characterized by rela- tively large edifices built by multiple eruptions over longer periods of time involving magmas with diverse origins. Eruption styles of small-scale volcanoes range from pyroclastic to effusive, and are strongly controlled by the relative influence of the characteristics of the magmatic system and the surface environment. Gold Open Access: This article is published under the terms of the CC-BY 3.0 license. Small-scale basaltic magmatic systems characteris- hazards associated with eruptions, and this is tically occur at the Earth’s surface as fields of small particularly true where volcanic fields are in close monogenetic volcanoes. These volcanoes are the proximity to population centres. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
11 Fall Unamagazine
FALL 2011 • VOLUME 19 • No. 3 FOR ALUMNI AND FRIENDS OF THE UNIVERSITY OF NORTH ALABAMA Cover Story 10 ..... Thanks a Million, Harvey Robbins Features 3 ..... The Transition 14 ..... From Zero to Infinity 16 ..... Something Special 20 ..... The Sounds of the Pride 28 ..... Southern Laughs 30 ..... Academic Affairs Awards 33 ..... Excellence in Teaching Award 34 ..... China 38 ..... Words on the Breeze Departments 2 ..... President’s Message 6 ..... Around the Campus 45 ..... Class Notes 47 ..... In Memory FALL 2011 • VOLUME 19 • No. 3 for alumni and friends of the University of North Alabama president’s message ADMINISTRATION William G. Cale, Jr. President William G. Cale, Jr. The annual everyone to attend one of these. You may Vice President for Academic Affairs/Provost Handy festival contact Dr. Alan Medders (Vice President John Thornell is drawing large for Advancement, [email protected]) Vice President for Business and Financial Affairs crowds to the many or Mr. Mark Linder (Director of Athletics, Steve Smith venues where music [email protected]) for information or to Vice President for Student Affairs is being played. At arrange a meeting for your group. David Shields this time of year Sometimes we measure success by Vice President for University Advancement William G. Cale, Jr. it is impossible the things we can see, like a new building. Alan Medders to go anywhere More often, though, success happens one Vice Provost for International Affairs in town and not hear music. The festival student at a time as we provide more and Chunsheng Zhang is also a reminder that we are less than better educational opportunities. -
Workshop on the Martiannorthern Plains: Sedimentological,Periglacial, and Paleoclimaticevolution
NASA-CR-194831 19940015909 WORKSHOP ON THE MARTIANNORTHERN PLAINS: SEDIMENTOLOGICAL,PERIGLACIAL, AND PALEOCLIMATICEVOLUTION MSATT ..V",,2' :o_ MarsSurfaceandAtmosphereThroughTime Lunar and PlanetaryInstitute 3600 Bay AreaBoulevard Houston TX 77058-1113 ' _ LPI/TR--93-04Technical, Part 1 Report Number 93-04, Part 1 L • DISPLAY06/6/2 94N20382"£ ISSUE5 PAGE2088 CATEGORY91 RPT£:NASA-CR-194831NAS 1.26:194831LPI-TR-93-O4-PT-ICNT£:NASW-4574 93/00/00 29 PAGES UNCLASSIFIEDDOCUMENT UTTL:Workshopon the MartianNorthernPlains:Sedimentological,Periglacial, and PaleoclimaticEvolution TLSP:AbstractsOnly AUTH:A/KARGEL,JEFFREYS.; B/MOORE,JEFFREY; C/PARKER,TIMOTHY PAA: A/(GeologicalSurvey,Flagstaff,AZ.); B/(NationalAeronauticsand Space Administration.GoddardSpaceFlightCenter,Greenbelt,MD.); C/(Jet PropulsionLab.,CaliforniaInst.of Tech.,Pasadena.) PAT:A/ed.; B/ed.; C/ed. CORP:Lunarand PlanetaryInst.,Houston,TX. SAP: Avail:CASIHC A03/MFAOI CIO: UNITEDSTATES Workshopheld in Fairbanks,AK, 12-14Aug.1993;sponsored by MSATTStudyGroupandAlaskaUniv. MAJS:/*GLACIERS/_MARSSURFACE/*PLAINS/*PLANETARYGEOLOGY/*SEDIMENTS MINS:/ HYDROLOGICALCYCLE/ICE/MARS CRATERS/MORPHOLOGY/STRATIGRAPHY ANN: Papersthathavebeen acceptedforpresentationat the Workshopon the MartianNorthernPlains:Sedimentological,Periglacial,and Paleoclimatic Evolution,on 12-14Aug. 1993in Fairbanks,Alaskaare included.Topics coveredinclude:hydrologicalconsequencesof pondedwateron Mars; morpho!ogical and morphometric studies of impact cratersin the Northern Plainsof Mars; a wet-geology and cold-climateMarsmodel:punctuation -
“Mining” Water Ice on Mars an Assessment of ISRU Options in Support of Future Human Missions
National Aeronautics and Space Administration “Mining” Water Ice on Mars An Assessment of ISRU Options in Support of Future Human Missions Stephen Hoffman, Alida Andrews, Kevin Watts July 2016 Agenda • Introduction • What kind of water ice are we talking about • Options for accessing the water ice • Drilling Options • “Mining” Options • EMC scenario and requirements • Recommendations and future work Acknowledgement • The authors of this report learned much during the process of researching the technologies and operations associated with drilling into icy deposits and extract water from those deposits. We would like to acknowledge the support and advice provided by the following individuals and their organizations: – Brian Glass, PhD, NASA Ames Research Center – Robert Haehnel, PhD, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory – Patrick Haggerty, National Science Foundation/Geosciences/Polar Programs – Jennifer Mercer, PhD, National Science Foundation/Geosciences/Polar Programs – Frank Rack, PhD, University of Nebraska-Lincoln – Jason Weale, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory Mining Water Ice on Mars INTRODUCTION Background • Addendum to M-WIP study, addressing one of the areas not fully covered in this report: accessing and mining water ice if it is present in certain glacier-like forms – The M-WIP report is available at http://mepag.nasa.gov/reports.cfm • The First Landing Site/Exploration Zone Workshop for Human Missions to Mars (October 2015) set the target -
Signs of Transport of Chemical Elements and Soil-Forming Processes in Surface Soils at Gale Crater, Mars E.M
47th Lunar and Planetary Science Conference (2016) 2493.pdf SIGNS OF TRANSPORT OF CHEMICAL ELEMENTS AND SOIL-FORMING PROCESSES IN SURFACE SOILS AT GALE CRATER, MARS E.M. Hausrath1, W. Goetz2, A. Cousin3, R.C. Wiens4, P.-Y. Mes- lin3, W. Rapin3 1UNLV, Las Vegas, NV [email protected] 2MPS, Göttingen, Germany 3IRAP, CNRS/UPS, Toulouse, France 4LANL, Los Alamos, NM Introduction: Soils provide an integrated record of martian surface processes. Recorded in soils is in- formation about parent material, the effect of impacts, aeolian and fluvial transport, chemical weathering from both ancient and modern Mars, and addition and loss of material. Analysis of soils can therefore provide important information about the history of Mars. Soil-forming processes in desert soils on Earth are preserved in the chemistry and morphology of those soils. Desert soils often contain desert pavement, an interlocking layer of rocks on the surface of the soil, and a dust-rich layer termed the Av horizon beneath the desert pavement [1]. Desert pavement can indicate age, with a more interlocking pavement indicating greater age [2]. Increasing age also results in a thicker dust-rich layer (Av horizon) beneath the desert pave- ment [2]. This dust-rich layer preserves not only the composition of the deposited aeolian dust, but also evidence of any interactions with liquid water. The Figure 1. NavCam image of the target Soda (indicated dust-rich layer also strongly affects how liquid water with a circle) Image credit: NASA/JPL-Caltech interacts with soils. Soils on Earth, including desert soils, can be stud- ied by analyzing depth profiles such as in soil pits or augered samples. -
Lunar Crater Volcanic Field (Reveille and Pancake Ranges, Basin and Range Province, Nevada, USA)
Research Paper GEOSPHERE Lunar Crater volcanic field (Reveille and Pancake Ranges, Basin and Range Province, Nevada, USA) 1 2,3 4 5 4 5 1 GEOSPHERE; v. 13, no. 2 Greg A. Valentine , Joaquín A. Cortés , Elisabeth Widom , Eugene I. Smith , Christine Rasoazanamparany , Racheal Johnsen , Jason P. Briner , Andrew G. Harp1, and Brent Turrin6 doi:10.1130/GES01428.1 1Department of Geology, 126 Cooke Hall, University at Buffalo, Buffalo, New York 14260, USA 2School of Geosciences, The Grant Institute, The Kings Buildings, James Hutton Road, University of Edinburgh, Edinburgh, EH 3FE, UK 3School of Civil Engineering and Geosciences, Newcastle University, Newcastle, NE1 7RU, UK 31 figures; 3 tables; 3 supplemental files 4Department of Geology and Environmental Earth Science, Shideler Hall, Miami University, Oxford, Ohio 45056, USA 5Department of Geoscience, 4505 S. Maryland Parkway, University of Nevada Las Vegas, Las Vegas, Nevada 89154, USA CORRESPONDENCE: gav4@ buffalo .edu 6Department of Earth and Planetary Sciences, 610 Taylor Road, Rutgers University, Piscataway, New Jersey 08854-8066, USA CITATION: Valentine, G.A., Cortés, J.A., Widom, ABSTRACT some of the erupted magmas. The LCVF exhibits clustering in the form of E., Smith, E.I., Rasoazanamparany, C., Johnsen, R., Briner, J.P., Harp, A.G., and Turrin, B., 2017, overlapping and colocated monogenetic volcanoes that were separated by Lunar Crater volcanic field (Reveille and Pancake The Lunar Crater volcanic field (LCVF) in central Nevada (USA) is domi variable amounts of time to as much as several hundred thousand years, but Ranges, Basin and Range Province, Nevada, USA): nated by monogenetic mafic volcanoes spanning the late Miocene to Pleisto without sustained crustal reservoirs between the episodes. -
Earth/Mars Comparison of Geological Features
Earth/Mars Comparison of Geological Features Objective(s): • Students will use satellite images to observe and compare various geological features between the planets Earth and Mars. • Students will work in groups to simulate and reproduce one of the geological features that they observed in the satellite images. • Students will use observational data from the experiment to conclude that some of the geological features on Mars could have been formed by flowing water. National Science Education Standards: • Content Standard D Grades 5 – 8: Earth’s History • Content Standard F Grades 5 – 8: Science and Technology in Society • Content Standard G Grades 5 – 8: Science as a Human Endeavor and Nature of Science Background: In this lesson, students explore the landforms of both Earth and Mars by carefully examining satellite images. The role of the student is to compare these landforms and share their observations with the class. Noting the similarities and the differences, the teacher then has the students focus on particular landforms on Mars – the channels and valley features. After discussing possible explanations for these features, the teacher introduces the stream tray investigation and the students conduct the experiment. Afterward, the students compare their data to several more images taken of Mars and conclude that these landforms could be the result of water having once flowed across A the planet’s surface. 2.5 km (1.6 mi) NAS “Did water once flow across the surface of Mars?” is a question Figure 1. This image taken from that scientists are still struggling to answer. A great deal of the Mars Global Surveyor using the evidence leads many to believe that water did indeed exist on Mars Orbiter Camera reveals a 9.8 Mars. -
{PDF EPUB} the War of the Worlds by HG Wells
Read Ebook {PDF EPUB} The War of the Worlds by H.G. Wells The War of the Worlds. Read summaries of H.G. Wells's The War of the Worlds . You can read a Plot Overview of the entire novel as well as Chapter-by-Chapter Summaries . To purchase a copy of The War of the Worlds on BN.com, go to the link below. Summary. Read a Plot Overview or Chapter-by-Chapter summaries of The War of the Worlds . Plot Overview Chapter Summaries. Teacher's Handbook. Teachers, check out our ideas for how you can creatively incorporate SparkNotes materials into your classroom instruction. The War of the Worlds. Our editors will review what you’ve submitted and determine whether to revise the article. The War of the Worlds , science fiction novel by H.G. Wells, first published serially by Pearson’s Magazine in the U.K. and by The Cosmopolitan magazine in the U.S. in 1897. The novel details a catastrophic conflict between humans and extraterrestrial “Martians.” It is considered a landmark work of science fiction, and it has inspired numerous adaptations and imitations. Plot summary. The War of the Worlds chronicles the events of a Martian invasion as experienced by an unidentified male narrator and his brother. The story begins a few years before the invasion. During the astronomical opposition of 1894, when Mars is closer to Earth than usual, several observatories spot flashes of light on the surface of Mars. The narrator witnesses one of these flashes through a telescope at an observatory in Ottershaw, Surrey, England. -
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Index [Italic page numbers indicate major references] Abajo Mountains, 382, 388 Amargosa River, 285, 309, 311, 322, Arkansas River, 443, 456, 461, 515, Abort Lake, 283 337, 341, 342 516, 521, 540, 541, 550, 556, Abies, 21, 25 Amarillo, Texas, 482 559, 560, 561 Abra, 587 Amarillo-Wichita uplift, 504, 507, Arkansas River valley, 512, 531, 540 Absaroka Range, 409 508 Arlington volcanic field, 358 Acer, 21, 23, 24 Amasas Back, 387 Aromas dune field, 181 Acoma-Zuni scction, 374, 379, 391 Ambrose tenace, 522, 523 Aromas Red Sand, 180 stream evolution patterns, 391 Ambrosia, 21, 24 Arroyo Colorado, 395 Aden Crater, 368 American Falls Lava Beds, 275, 276 Arroyo Seco unit, 176 Afton Canyon, 334, 341 American Falls Reservoir, 275, 276 Artemisia, 21, 24 Afton interglacial age, 29 American River, 36, 165, 173 Ascension Parish, Louisana, 567 aggradation, 167, 176, 182, 226, 237, amino acid ash, 81, 118, 134, 244, 430 323, 336, 355, 357, 390, 413, geochronology, 65, 68 basaltic, 85 443, 451, 552, 613 ratios, 65 beds, 127,129 glaciofluvial, 423 aminostratigraphy, 66 clays, 451 Piedmont, 345 Amity area, 162 clouds, 95 aggregate, 181 Anadara, 587 flows, 75, 121 discharge, 277 Anastasia Formation, 602, 642, 647 layer, 10, 117 Agua Fria Peak area, 489 Anastasia Island, 602 rhyolitic, 170 Agua Fria River, 357 Anchor Silt, 188, 198, 199 volcanic, 54, 85, 98, 117, 129, Airport bench, 421, 423 Anderson coal, 448 243, 276, 295, 396, 409, 412, Alabama coastal plain, 594 Anderson Pond, 617, 618 509, 520 Alamosa Basin, 366 andesite, 75, 80, 489 Ash Flat, 364 Alamosa -
Geomorphological Evolution and Chronology of the Eruptive Activity of the Columba and Cuevas Volcanoes (Campo De Calatrava Volcanic Field, Ciudad Real, Central Spain)
Accepted Manuscript Geomorphological evolution and chronology of the eruptive activity of the Columba and Cuevas volcanoes (Campo de Calatrava Volcanic Field, Ciudad Real, Central Spain) Miguel Ángel Poblete Piedrabuena, Joan Martí Molist, Salvador Beato Bergua, José Luis Marino Alfonso PII: S0169-555X(19)30125-4 DOI: https://doi.org/10.1016/j.geomorph.2019.03.026 Reference: GEOMOR 6720 To appear in: Geomorphology Received date: 4 December 2018 Revised date: 14 March 2019 Accepted date: 25 March 2019 Please cite this article as: M.Á.P. Piedrabuena, J.M. Molist, S.B. Bergua, et al., Geomorphological evolution and chronology of the eruptive activity of the Columba and Cuevas volcanoes (Campo de Calatrava Volcanic Field, Ciudad Real, Central Spain), Geomorphology, https://doi.org/10.1016/j.geomorph.2019.03.026 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. ACCEPTED MANUSCRIPT Geomorphological evolution and chronology of the eruptive activity of the Columba and Cuevas volcanoes (Campo de Calatrava Volcanic Field, Ciudad Real, Central Spain) Miguel Ángel Poblete Piedrabuena1*, Joan Martí Molist2, Salvador Beato Bergua1, José Luis Marino Alfonso1 Department of Geography, University of Oviedo, Campus de El Milán, C/Amparo Pedregal, 5, Oviedo-33011, Spain.