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Enceladus, Moon of Saturn
National Aeronautics and and Space Space Administration Administration Enceladus, Moon of Saturn www.nasa.gov Enceladus (pronounced en-SELL-ah-dus) is an icy moon of Saturn with remarkable activity near its south pole. Covered in water ice that reflects sunlight like freshly fallen snow, Enceladus reflects almost 100 percent of the sunlight that strikes it. Because the moon reflects so much sunlight, the surface temperature is extremely cold, about –330 degrees F (–201 degrees C). The surface of Enceladus displays fissures, plains, corrugated terrain and a variety of other features. Enceladus may be heated by a tidal mechanism similar to that which provides the heat for volca- An artist’s concept of Saturn’s rings and some of the icy moons. The ring particles are composed primarily of water ice and range in size from microns to tens of meters. In 2004, the Cassini spacecraft passed through the gap between the F and G rings to begin orbiting Saturn. noes on Jupiter’s moon Io. A dramatic plume of jets sprays water ice and gas out from the interior at ring material, coating itself continually in a mantle Space Agency. The Jet Propulsion Laboratory, a many locations along the famed “tiger stripes” at of fresh, white ice. division of the California Institute of Technology, the south pole. Cassini mission data have provided manages the mission for NASA. evidence for at least 100 distinct geysers erupting Saturn’s Rings For images and information about the Cassini on Enceladus. All of this activity, plus clues hidden Saturn’s rings form an enormous, complex struc- mission, visit — http://saturn.jpl.nasa.gov/ in the moon’s gravity, indicates that the moon’s ture. -
Appendix 1: Io's Hot Spots Rosaly M
Appendix 1: Io's hot spots Rosaly M. C. Lopes,Jani Radebaugh,Melissa Meiner,Jason Perry,and Franck Marchis Detections of plumes and hot spots by Galileo, Voyager, HST, and ground-based observations. Notes and sources . (N) NICMOS hot spots detected by Goguen etal . (1998). (D) Hot spots detected by C. Dumas etal . in 1997 and/or 1998 (pers. commun.). Keck are hot spots detected by de Pater etal . (2004) and Marchis etal . (2001) from the Keck telescope using Adaptive Optics. (V, G, C) indicate Voyager, Galileo,orCassini detection. Other ground-based hot spots detected by Spencer etal . (1997a). Galileo PPR detections from Spencer etal . (2000) and Rathbun etal . (2004). Galileo SSIdetections of hot spots, plumes, and surface changes from McEwen etal . (1998, 2000), Geissler etal . (1999, 2004), Kezthelyi etal. (2001), and Turtle etal . (2004). Galileo NIMS detections prior to orbit C30 from Lopes-Gautier etal . (1997, 1999, 2000), Lopes etal . (2001, 2004), and Williams etal . (2004). Locations of surface features are approximate center of caldera or feature. References de Pater, I., F. Marchis, B. A. Macintosh, H. G. Rose, D. Le Mignant, J. R. Graham, and A. G. Davies. 2004. Keck AO observations of Io in and out of eclipse. Icarus, 169, 250±263. 308 Appendix 1: Io's hot spots Goguen, J., A. Lubenow, and A. Storrs. 1998. HST NICMOS images of Io in Jupiter's shadow. Bull. Am. Astron. Assoc., 30, 1120. Geissler, P. E., A. S. McEwen, L. Keszthelyi, R. Lopes-Gautier, J. Granahan, and D. P. Simonelli. 1999. Global color variations on Io. Icarus, 140(2), 265±281. -
Final Report of the Opgt/Mjs Plasma Wave Science Team
1 September 1972 FINAL REPORT OF THE OPGT/MJS PLASMA WAVE SCIENCE TEAM Prepared by F. L. Scarf, Team Leader for National Aeronautical and Space Administration Washington, D.C. 205*t6 Contract NASW 2228 Space Sciences Department TRW Systems Group One Space Park Redondo Beach, California 902?8 4 Page 1 1. TEAM ORGANIZATION AND MEMBERSHIP The Plasma Wave Team Leader is Dr. F. L. Scarf of TRW Systems, and the official team members are Dr. D. A. Gurnett (University of Iowa), Dr. R. A. Helliwell (Stanford University), Dr. R. E. Holzer (UCLA), Dr. P. J. Kellogg (University of Minnesota), Dr. E. J. Smith (JPL), and Dr. E. Ungstrup (Danish Space Research Institute). Mr. A. M. A. Frandsen of JPL serves as Team Member and Experiment Representative. In addition, the Plasma Wave Team solicited the continuing support and assistance of several other outstanding scientists, and we have designated these participants as Team Associates; the Associates are Dr. N. M. Brice (Cornell University), Dr. D. Cartwright (University of Minnesota), Dr. R. W. Fredricks (TRW), Dr. H. B. Liemohn (Boeing), Dr. C. F. Kennel (UCLA), and Dr. R. Thome (UCLA) . 2. GENERAL TEAM ACTIVITIES FEBRUARY 1972-AUGUST 31, 1972 (See the mid-year report for a summary of the earlier work) During this period Dr. Scarf attended all SSG Meetings except the last one, where Dr. E. J. Smith represented the Plasma Wave Team. There were a number of Team Meetings and several additional .conferences at JPL concerning EMI and other potential spacecraft problems. The major development during this interval involved the decision not to go ahead with the Grand Tour. -
1783-84 Laki Eruption, Iceland
1783-84 Laki eruption, Iceland Eruption History and Atmospheric Effects Thor Thordarson Faculty of Earth sciences, University of Iceland 12/8/2017 1 Atmospheric Effects of the 1783-84 Laki Eruption in Iceland Outline . Volcano-Climate interactions - background Laki eruption . Eruption history . Sulfur release and aerosol loading . Plume transport and aerosol dispersal . Environmental and climatic effects 12/8/2017. Concluding Remarks 2 Santorini, 1628 BC Tambora, 1815 Etna, 44 BC Lakagígar, 1783 Toba, 71,000 BP Famous Volcanic Eruptions Krakatau, 1883 Pinatubo, 1991 El Chichón, 1982 Agung, 1963 St. Helens, 1980 Major volcanic eruptions of the past 250 years Volcano Year VEI d.v.i/Emax IVI Lakagígar [Laki craters], Iceland 1783 4 2300 0.19 Unknown (El Chichón?) 1809 0.20 Tambora, Sumbawa, Indonesia 1815 7 3000 0.50 Cosiguina, Nicaragua 1835 5 4000 0.11 Askja, Iceland 1875 5 1000 0.01* Krakatau, Indonesia 1883 6 1000 0.12 Okataina [Tarawera], North Island, NZ 1886 5 800 0.04 Santa Maria, Guatemala 1902 6 600 0.05 Ksudach, Kamchatka, Russia 1907 5 500 0.02 Novarupta [Katmai], Alaska, US 1912 6 500 0.15 Agung, Bali, Indonesia 1963 4 800 0.06 Mt. St. Helens, Washington, US 1980 5 500 0.00 El Chichón, Chiapas, Mexico 1982 5 800 0.06 Mt. Pinatubo, Luzon, Philippines 1991 6 1000 — Volcano – Climate Interactions Key to Volcanic Forcing is: SO2 mass loading, eruption duration plume height replenishment aerosol production, residence time 12/8/2017 5 Volcanic Forcing: sulfur dioxide sulfate aerosols SO2 75%H2SO4+ 25%H2O clear sky 1991 Pinatubo aerosols -
Jacques Tiziou Space Collection
Jacques Tiziou Space Collection Isaac Middleton and Melissa A. N. Keiser 2019 National Air and Space Museum Archives 14390 Air & Space Museum Parkway Chantilly, VA 20151 [email protected] https://airandspace.si.edu/archives Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Biographical / Historical.................................................................................................... 1 Scope and Contents........................................................................................................ 2 Arrangement..................................................................................................................... 2 Names and Subjects ...................................................................................................... 2 Container Listing ............................................................................................................. 4 Series : Files, (bulk 1960-2011)............................................................................... 4 Series : Photography, (bulk 1960-2011)................................................................. 25 Jacques Tiziou Space Collection NASM.2018.0078 Collection Overview Repository: National Air and Space Museum Archives Title: Jacques Tiziou Space Collection Identifier: NASM.2018.0078 Date: (bulk 1960s through -
A Pictorial History of Rockets
he mighty space rockets of today are the result A Pictorial Tof more than 2,000 years of invention, experi- mentation, and discovery. First by observation and inspiration and then by methodical research, the History of foundations for modern rocketry were laid. Rockets Building upon the experience of two millennia, new rockets will expand human presence in space back to the Moon and Mars. These new rockets will be versatile. They will support Earth orbital missions, such as the International Space Station, and off- world missions millions of kilometers from home. Already, travel to the stars is possible. Robotic spacecraft are on their way into interstellar space as you read this. Someday, they will be followed by human explorers. Often lost in the shadows of time, early rocket pioneers “pushed the envelope” by creating rocket- propelled devices for land, sea, air, and space. When the scientific principles governing motion were discovered, rockets graduated from toys and novelties to serious devices for commerce, war, travel, and research. This work led to many of the most amazing discoveries of our time. The vignettes that follow provide a small sampling of stories from the history of rockets. They form a rocket time line that includes critical developments and interesting sidelines. In some cases, one story leads to another, and in others, the stories are inter- esting diversions from the path. They portray the inspirations that ultimately led to us taking our first steps into outer space. NASA’s new Space Launch System (SLS), commercial launch systems, and the rockets that follow owe much of their success to the accomplishments presented here. -
America's Greatest Projects and Their Engineers - VII
America's Greatest Projects and Their Engineers - VII Course No: B05-005 Credit: 5 PDH Dominic Perrotta, P.E. Continuing Education and Development, Inc. 22 Stonewall Court Woodcliff Lake, NJ 076 77 P: (877) 322-5800 [email protected] America’s Greatest Projects & Their Engineers-Vol. VII The Apollo Project-Part 1 Preparing for Space Travel to the Moon Table of Contents I. Tragedy and Death Before the First Apollo Flight A. The Three Lives that Were Lost B. Investigation, Findings & Recommendations II. Beginning of the Man on the Moon Concept A. Plans to Land on the Moon B. Design Considerations and Decisions 1. Rockets – Launch Vehicles 2. Command/Service Module 3. Lunar Module III. NASA’s Objectives A. Unmanned Missions B. Manned Missions IV. Early Missions V. Apollo 7 Ready – First Manned Apollo Mission VI. Apollo 8 - Orbiting the Moon 1 I. Tragedy and Death Before the First Apollo Flight Everything seemed to be going well for the Apollo Project, the third in a series of space projects by the United States intended to place an American astronaut on the Moon before the end of the 1960’s decade. Apollo 1, known at that time as AS (Apollo Saturn)-204 would be the first manned spaceflight of the Apollo program, and would launch a few months after the flight of Gemini 12, which had occurred on 11 November 1966. Although Gemini 12 was a short duration flight, Pilot Buzz Aldrin had performed three extensive EVA’s (Extra Vehicular Activities), proving that Astronauts could work for long periods of time outside the spacecraft. -
Contents More Information
Cambridge University Press 978-0-521-85003-2 - Volcanism on Io: A Comparison with Earth Ashley Gerard Davies Table of Contents More information Contents Preface page xi List of Abbreviations xiii Reproduction Permissions xv Introduction 1 Section 1 Io, 1610 to 1995: Galileo to Galileo 1 Io, 1610–1979 7 1.1 Io before Voyager 7 1.2 Prediction of volcanic activity 9 1.3 Voyager to Jupiter 9 1.4 Discovery of active volcanism 12 1.5 IRIS and volcanic thermal emission 18 1.6 Io: the view after Voyager 19 1.7 Summary 24 2 Between Voyager and Galileo: 1979–1995 27 2.1 Silicate volcanism on Io? 27 2.2 Ground-based observations 29 2.3 Observations of Io from Earth orbit 33 2.4 The Pele plume 33 2.5 Outburst eruptions 34 2.6 Stealth plumes 37 2.7 Io on the eve of Galileo 38 3 Galileo at Io 39 3.1 Instrumentation 41 3.2 Galileo observations of Io 46 Section 2 Planetary volcanism: evolution and composition 4 Io and Earth: formation, evolution, and interior structure 53 4.1 Global heat flow 53 4.2 Planetary formation 55 v © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-85003-2 - Volcanism on Io: A Comparison with Earth Ashley Gerard Davies Table of Contents More information vi Contents 4.3 Post-formation heating 58 4.4 Interior structure 63 4.5 Volcanism over time 70 4.6 Implications 72 5 Magmas and volatiles 73 5.1 Basalt 73 5.2 Ultramafic magma 74 5.3 Lava rheology 76 5.4 Sulphur 78 5.5 Sulphur dioxide (SO2)86 Section 3 Observing and modeling volcanic activity 6 Observations: thermal remote sensing -
Page 1 57° 50° 40° 30° 20° 10° 0° -10° -20° -30° -40° -50° -57° 57° 50
180° 0° DODONA PLANUM 210° 330° 150° 30° 60° -60° . Bochica . Hatchawa Patera Patera . Nusku Patera . Hiruko Heno . Inti . Patera Patera Patera 70° -70° 240° 300° 60° 120° Tvashtar . Taranis Patera Iynx TARSUS Aramazd Mensa . Patera Tvashtar Paterae Haemus REGIO Montes Mensae LERNA REGIO 80° Echo -80°Mensa . Chors Nile Montes N Patera E M . Viracocha E Patera A 90° CHALYBES 270° 90° P 270° L A . Mithra N Patera U REGIO M . Vivasvant Patera . Crimea Mons 80° -80° Pyerun . Patera Dazhbog 120° 60° Patera . 300° 240° 70° -70° ILLYRIKON REGIO 60° -60° 30° 150° 330° 210° 0° 180° NORTH POLAR REGION SOUTH POLAR REGION 180° 170° 160° 150° 140° 130° 120° 110° 100° 90° 80° 70° 60° 50° 40° 30° 20° 10° 0° 350° 340° 330° 320° 310° 300° 290° 280° 270° 260° 250° 240° 230° 220° 210° 200° 190° 180° 57° 57° Nile Montes Dazhbog Patera CHALYBES REGIO 50° 50° . Kinich Ahau . Savitr Patera Patera Surt Zal Montes Lei-Kung Zal Fluctus . Fo Patera 40° 40° Patera Thor . Amaterasu . Dusura Patera Patera BULICAME . Manua Patera Shango REGIO Arinna . _ Patera Ukko . Atar Fluctus . Patera Patera Heiseb Isum 30° . 30° Fuchi Patera Patera Reshef Euxine . Patera Mons Patera Volund . Thomagata Amirani Patera . Shakuru Skythia Mons Girru . Mongibello . Tiermes Patera . Susanoo Donar Surya Estan Patera Patera . Patera Mons Patera Fluctus Patera Monan Daedalus 20° . Patera Loki . 20° Zamama Maui . Gish Bar Patera Mons Mulungu Steropes Maui . Patera . Patera Ruaumoko . Camaxtli Patera Gish Bar Sobo Patera . Patera Patera Fluctus Monan Loki Chaac . Ababinili Tien Mu Mons Llew . Balder Patera . Fjorgynn Patera . -
N AS a Facts
National Aeronautics and Space Administration NASA’s Launch Services Program he Launch Services Program (LSP) manufacturing, launch operations and rockets for launching Earth-orbit and Twas established at Kennedy Space countdown management, and providing interplanetary missions. Center for NASA’s acquisition and added quality and mission assurance in In September 2010, NASA’s Launch program management of expendable lieu of the requirement for the launch Services (NLS) contract was extended launch vehicle (ELV) missions. A skillful service provider to obtain a commercial by the agency for 10 years, through NASA/contractor team is in place to launch license. 2020, with the award of four indefinite meet the mission of the Launch Ser- Primary launch sites are Cape Canav- delivery/indefinite quantity contracts. The vices Program, which exists to provide eral Air Force Station (CCAFS) in Florida, expendable launch vehicles that NASA leadership, expertise and cost-effective and Vandenberg Air Force Base (VAFB) has available for its science, Earth-orbit services in the commercial arena to in California. and interplanetary missions are United satisfy agencywide space transporta- Other launch locations are NASA’s Launch Alliance’s (ULA) Atlas V and tion requirements and maximize the Wallops Flight Facility in Virginia, the Delta II, Space X’s Falcon 1 and 9, opportunity for mission success. Kwajalein Atoll in the South Pacific’s Orbital Sciences Corp.’s Pegasus and facts The principal objectives of the LSP Republic of the Marshall Islands, and Taurus XL, and Lockheed Martin Space are to provide safe, reliable, cost-effec- Kodiak Island in Alaska. Systems Co.’s Athena I and II. -
Roger Angel University of Arizona
NIAC Fellows meeting Atlanta March 7 2007 Phase I report Practicality of a solar shield in space to counter global warming Roger Angel University of Arizona Pete Worden and Kevin Parkin NASA Ames Research Center Dave Miller MIT Planet Earth driver’s test 1) You are zipping along happily, when you see warning lights ahead in the distance but visibility is not so great. What should you do? a) Just floor it b) take you foot off the accelerator c) apply the brakes 2) You find you have no brakes. What should you do now? The warning CO2 in atmosphere works just like water vapor • Lets in warming sunlight in the day • when humidity is high heat is trapped and nights stay warm • when humidity is low heat escapes and nights are cold • But unlike water vapor, CO2 hangs around – added CO2 in the atmosphere takes a century or two to dissipate Geoengineering solutions could be really useful • Needed if current CO2 level already beyond “tipping point” • Even extreme conservation may not be able to stop abrupt and disastrous changes e.g. – changes in ocean circulation – Greenland melts (20’ permanent sea level rise) • Many leading scientists seriously worried • Probability of disaster 10% - 20%? – Geoengineering like taking out insurance against unlikely but catastrophic event) Geoengineering has been taboo • People worry it will take off the pressure for permanent solution of not burning fossil fuel – Administration pointed to possibility of geoengineering and space mirrors just before recent IPCC report • If used for an extended period, would lead to seriously unstable planet Earth, ever more hooked on carbon • But if we don’t look at it, we have no insurance Heating reversible by reducing solar flux • Govindasamy, B. -
Submarine Growth of a Hawaiian Shield Volcano
SUBMARINE GROWTH OF A HAWAIIAN SHIELD VOLCANO BASED ON VOLCANICLASTICS IN THE HAWAIIAN SCIENTIFIC DRILLING PROJECT 2 CORE A THESIS SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI'I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE IN GEOLOGY & GEOPHYSICS DECEMBER 2004 By Kate Phillippa Bridges Thesis Committee: Michael O. Garcia, Chairperson Bruce Houghton Thor Thordarson ACKNOWLEDGEMENTS I would like to thank my teachers and colleagues at the University of Hawai'i at Manoa Geology and Geophysics department for their inspiration and encouragement. In particular, I would like to thank Mike Garcia for giving me the opportunity to pursue and complete a Master's degree in volcanology at the University of Hawai'i. In addition, I am very grateful for all the support he has given me throughout the past three years and his sense of humor. Mahalos also to Thor Thordarsen, who always had words of encouragement to accompany his insightful comments on the progress and outcome of this study. Thanks to Bruce Houghton for sound scientific advise and guidance. Finally, muchos mahalos to all my friends for making the journey to Masterhood fun and, of course, to my folks! iii Acknowledgements iii List of figures vii List of tables viii Abstract ix 1. INTRODUCTION 1 1.1 Geological setting 2 1.2 Models for the growth of shield volcanoes 4 1.2.1 Magma supply and stages 4 1.2.2 Deposits 5 1.2.3 Subsidence and collapse ..7 1.3 Hawaiian Scientific Drilling Project 9 1.3.1 Introduction, 9 1.3.2 Basic stratigraphy of the HSDP2 core .11 1.3.3 Introduction to the HSDP2 volcaniclastics 14 1.4 Terminology 21 1.5 Subaqueous fragmentation of basaltic magma 23 1.5.1 Magmatic explosivity 23 1.5.2 Steam explosivity 24 Littoral magma:water interaction Subaqueous magma:water interaction 1.5.3 Passive quenching and autobrecciation of lava ~ 29 1.5.4 Secondary fragmentation of basaltic magma 29 2.