The Upper Atmosphere of Jupiter*
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Ozone Layer Depletion (PDF)
United States Air and Radiation EPA 430-F-10-027 Environmental Protection 6205J August 2010 Agency www.epa.gov/ozone/strathome.html Ozone Layer Depletion The stratospheric ozone layer forms a thin shield in the upper atmosphere, protecting life on Earth from the sun’s ultraviolet (UV) rays. It has been called the Earth’s sunscreen. In the 1980s, scientists found evidence that the ozone layer was being depleted. Depletion of the ozone layer results in increased UV radiation reaching the Earth’s surface, which in turn leads to a greater chance of overexposure to UV radiation and the related health effects of skin cancer, cataracts, and immune suppression. This fact sheet explains the importance of protecting the stratospheric ozone layer. What is Stratospheric Ozone? Ozone is a naturally-occurring gas that can be good or bad for your health and the environment depending on its location in the atmosphere. In the layer near the Earth’s surface—the troposphere— ground-level or “bad” ozone is an air pollutant that is a key ingredient of urban smog. But higher up, in the stratosphere, “good” ozone protects life on Earth by absorbing some of the sun’s UV rays. An easy way to remember this is the phrase “good up high, bad nearby.” Ozone Layer Depletion Compounds that contain chlorine and bromine molecules, such as methyl chloroform, halons, and chlorofluorocarbons (CFCs), are stable and have atmospheric lifetimes long enough to be transported by winds into Ozone “up high” in the stratosphere protects the Earth, while ozone close to the Earth’s surface is harmful. -
Ira Sprague Bowen Papers, 1940-1973
http://oac.cdlib.org/findaid/ark:/13030/tf2p300278 No online items Inventory of the Ira Sprague Bowen Papers, 1940-1973 Processed by Ronald S. Brashear; machine-readable finding aid created by Gabriela A. Montoya Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 © 1998 The Huntington Library. All rights reserved. Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague 1 Bowen Papers, 1940-1973 Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague Bowen Paper, 1940-1973 The Huntington Library San Marino, California Contact Information Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 Processed by: Ronald S. Brashear Encoded by: Gabriela A. Montoya © 1998 The Huntington Library. All rights reserved. Descriptive Summary Title: Ira Sprague Bowen Papers, Date (inclusive): 1940-1973 Creator: Bowen, Ira Sprague Extent: Approximately 29,000 pieces in 88 boxes Repository: The Huntington Library San Marino, California 91108 Language: English. Provenance Placed on permanent deposit in the Huntington Library by the Observatories of the Carnegie Institution of Washington Collection. This was done in 1989 as part of a letter of agreement (dated November 5, 1987) between the Huntington and the Carnegie Observatories. The papers have yet to be officially accessioned. Cataloging of the papers was completed in 1989 prior to their transfer to the Huntington. -
Unser Sonnensystem
Deutsches Zentrum für Luft- und Raumfahrt e.V. Institut für Planetenforschung UNSER SONNENSYSTEM Kurzer Überblick über die Körper unseres Sonnensystems und deren Erkundung mit Raumsonden zusammengestellt von Susanne Pieth und Ulrich Köhler Regional Planetary Image Facility Direktor: Prof. Dr. Ralf Jaumann Datenmanager: Susanne Pieth 2017, 4., aktualisierte und erweiterte Auflage INHALT 3 Geleitwort 5 Exploration des Sonnensystems mit Raumsonden 11 Sonnensystem und vergleichende Planetologie 17 Sonne 21 Merkur 25 Venus 29 Erde-Mond-System 41 Mars 47 Asteroiden 55 Jupiter 61 Saturn 69 Uranus 73 Neptun 77 Kuipergürtel und Zwergplaneten 85 Kometen 93 Planetenentstehung und Leben 97 Extrasolare Planeten Anhang 100 Übersicht über die Missionen im Sonnensystem Impressum 119 Wie komme ich an Bilddaten? Herausgeber: Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR) Institut für Planetenforschung Regional Planetary Image Facility Die Texte entstanden unter Mitwirkung von Dr. Manfred Gaida, Anschrift: Dr. Christian Gritzner, Prof. Dr. Alan Harris, Ernst Hauber, Dr. Rutherfordstr. 2, 12489 Berlin Jörn Helbert, Prof. Dr. Harald Hiesinger, Dr. Hauke Hußmann, Telefon + 49 (030) 67055-333 Prof. Dr. Ralf Jaumann, Dr. Ekkehard Kührt, Dr. René Laufer, E-Mail [email protected] Dr. Stefano Mottola, Prof. Dr. Jürgen Oberst, Dr. Katharina DLR.de/rpif/ Otto, Dr. Ana-Catalina Plesa, Dr. Frank Sohl, Prof. Dr. Tilman Spohn, Dr. Alexander Stark, Dr. Katrin Stephan, Dr. Daniela Titelbild: DLR (CC-BY 3.0) Tirsch, Dr. Ruth Titz-Weider und Dr. Roland Wagner. Geleitwort GELEITWORT Eine Reise durch das Sonnensystem In der Natur von Forschung liegt es, dass mit jedem gelösten Rätsel neue Fragen aufgeworfen werden. Wie entstand das Leben auf der Im Jahr 1610 richtete Galileo Galilei zum ersten Mal den Blick durch Erde? Kommt es von einem anderen Himmelskörper oder wäre hö- ein Fernrohr auf die Gestirne – und entdeckte wahrlich „Revo- her entwickeltes Leben auf der Erde ohne den großen Mond denn lutionäres“. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 33: AUGUST 9-15 Presented by The Earthrise Institute # 33 Authored by Alan Hale About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets. -
Ozone: Good up High, Bad Nearby
actions you can take High-Altitude “Good” Ozone Ground-Level “Bad” Ozone •Protect yourself against sunburn. When the UV Index is •Check the air quality forecast in your area. At times when the Air “high” or “very high”: Limit outdoor activities between 10 Quality Index (AQI) is forecast to be unhealthy, limit physical exertion am and 4 pm, when the sun is most intense. Twenty minutes outdoors. In many places, ozone peaks in mid-afternoon to early before going outside, liberally apply a broad-spectrum evening. Change the time of day of strenuous outdoor activity to avoid sunscreen with a Sun Protection Factor (SPF) of at least 15. these hours, or reduce the intensity of the activity. For AQI forecasts, Reapply every two hours or after swimming or sweating. For check your local media reports or visit: www.epa.gov/airnow UV Index forecasts, check local media reports or visit: www.epa.gov/sunwise/uvindex.html •Help your local electric utilities reduce ozone air pollution by conserving energy at home and the office. Consider setting your •Use approved refrigerants in air conditioning and thermostat a little higher in the summer. Participate in your local refrigeration equipment. Make sure technicians that work on utilities’ load-sharing and energy conservation programs. your car or home air conditioners or refrigerator are certified to recover the refrigerant. Repair leaky air conditioning units •Reduce air pollution from cars, trucks, gas-powered lawn and garden before refilling them. equipment, boats and other engines by keeping equipment properly tuned and maintained. During the summer, fill your gas tank during the cooler evening hours and be careful not to spill gasoline. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
The Ozone Layer Our Global Sunscreen by Mike Carlowicz
The Ozone Layer Our Global Sunscreen By Mike Carlowicz t’s not often that scientists get to conduct experiments that seem like they come out of a A good idea with a science fiction novel or a video game. Yet, that is what some researchers at NASA did a few bad outcome years ago. Atmospheric physicists Paul Newman and Luke Oman built a simulation of the Earth’s The experiments run by Newman and atmosphere and then proceeded to strip away our protective ozone layer. Their computer colleagues were actually extensions of an model reproduced the chemistry and circulation of the air; natural variations in temperatures and experiment that humans have been unwit- winds; and minor changes in the energy received from the sun. Newman and Oman then added tingly running with Earth for nearly a cen- ozone-destroying chemicals to the atmosphere at a rate of 3% more per year—on top of what tury. Humans have been depleting the ozone was already in our 1970s atmosphere. For several months, they ran their model on a supercom- layer with chemical products. puter and reproduced about 80 years of simulated Earth time. They called their experiment “The The unintentional experiment started World Avoided.” in the late 1920s, when Thomas Midgley By the year 2020 in the simulation, 17% of the Earth’s protective ozone layer vanished. Holes Jr. and other industrial chemists began to in the ozone layer formed not just over Antarctica—as they currently do each spring—but over produce chlorofluorocarbons (CFCs), non- the Arctic, too. By 2040, the ultraviolet (UV) index, the measure of the sunburn-causing radiation toxic compounds that improved refrigera- reaching the Earth’s surface, rose as high as 15 on summer days in mid-latitude cities such as tion. -
UV Radiation (PDF)
United States Air and Radiation EPA 430-F-10-025 Environmental Protection 6205J June 2010 Agency www.epa.gov/ozone/strathome.html UV Radiation This fact sheet explains the types of ultraviolet radiation and the various factors that can affect the levels reaching the Earth’s surface. The sun emits energy over a broad spectrum of wavelengths: visible light that you see, infrared radiation that you feel as heat, and ultraviolet (UV) radiation that you can’t see or feel. UV radiation has a shorter wavelength and higher energy than visible light. It affects human health both positively and negatively. Short exposure to UVB radiation generates vitamin D, but can also lead to sunburn depending on an individual’s skin type. Fortunately for life on Earth, our atmosphere’s stratospheric ozone layer shields us from most UV radiation. What does get through the ozone layer, however, can cause the following problems, particularly for people who spend unprotected time outdoors: ● Skin cancer ● Suppression of the immune system ● Cataracts ● Premature aging of the skin Did You Since the benefits of sunlight cannot be separated from its damaging effects, it is important to understand the risks of overexposure, and take simple precautions to protect yourself. Know? Types of UV Radiation Ultraviolet (UV) radiation, from the Scientists classify UV radiation into three types or bands—UVA, UVB, and UVC. The ozone sun and from layer absorbs some, but not all, of these types of UV radiation: ● tanning beds, is UVA: Wavelength: 320-400 nm. Not absorbed by the ozone layer. classified as a ● UVB: Wavelength: 290-320 nm. -
Stratospheric Ozone Protection: 30 Years of Progress and Achievements
Stratospheric Ozone Protection: 30 Years of Progress and Achievements United States Environmental Protection Agency Office of Air and Radiation 1200 Pennsylvania Avenue, NW (6205T) Washington, DC 20460 https://www.epa.gov/ozone-layer-protection EPA-430-F-17-006 November 2017 Page 2 Stratospheric Ozone Protection 30 Years of Progress and Achievements Stratospheric Ozone Protection: 30 Years of Progress and Achievements Introduction Overexposure to ultraviolet (UV) radiation is a (CFCs), which were widely used in a variety of threat to human health. It can cause skin damage, industrial and household applications, such as eye damage, and even suppress the immune sys- aerosol sprays, plastic foams, and the refriger- tem. UV overexposure also interferes with envi- ant in refrigerators, air conditioning units in cars ronmental cycles, affecting organisms—such as and buildings, and elsewhere. plants and phytoplankton—that move nutrients and energy through the biosphere. Scientific observations of the rapid thinning of the ozone layer over Antarctica from the late In the 1970s, scientists discovered that Earth’s 1970s onward—often referred to as the “ozone primary protection from UV radiation, the strato- hole”—catalyzed international action to dis- spheric ozone layer, was thinning as a result of continue the use of CFCs. In 1987, the United the use of chemicals that contained chlorine States joined 23 other countries and the Euro- and bromine, which when broken down could pean Union to sign the Montreal Protocol on destroy ozone molecules. The -
The Arctic Ozone Layer
The Arctic Ozone Layer How the Arctic Ozone Layer is Responding to Ozone-Depleting Chemicals and Climate Change Photographs are the property of the EC ARQX picture archive. Special permission was obtained from Mike Harwood (p. vii: Muskoxen on Ellesmere Island), Richard Mittermeier (pp. vii, 12: Sunset from the Polar Environment Atmospheric Research Laboratory), Angus Fergusson (p. 4: Iqaluit; p. 8: Baffin Island), Yukio Makino (p. vii: Instrumentation and scientist on top of the Polar Environment Atmospheric Research Laboratory), Tomohiro Nagai (p. 25: Figure 20), and John Bird (p. 30: Polar Environment Atmospheric Research Laboratory). To obtain additional copies of this report, write to: Angus Fergusson Science Assessments Section Science & Technology Integration Division Environment Canada 4905 Dufferin Street Toronto ON M3H 5T4 Canada Please send feedback, comments and suggestions to [email protected] © Her Majesty the Queen in Right of Canada, represented by the Minister of the Environment, 2010. Catalogue No.: En164-18/2010E ISBN: 978-1-100-10787-5 Aussi disponible en français The Arctic Ozone Layer How the Arctic Ozone Layer is Responding to Ozone-Depleting Chemicals and Climate Change by Angus Fergusson Acknowledgements The author wishes to thank David Wardle, Ted Shepherd, Norm McFarlane, Nathan Gillett, John Scinocca, Darrell Piekarz, Ed Hare, Elizabeth Bush, Jacinthe Lacroix and Hans Fast for their valuable advice and assistance during the preparation of this manuscript. i Contents Summary .................................................................................................................................................... -
Index to JRASC Volumes 61-90 (PDF)
THE ROYAL ASTRONOMICAL SOCIETY OF CANADA GENERAL INDEX to the JOURNAL 1967–1996 Volumes 61 to 90 inclusive (including the NATIONAL NEWSLETTER, NATIONAL NEWSLETTER/BULLETIN, and BULLETIN) Compiled by Beverly Miskolczi and David Turner* * Editor of the Journal 1994–2000 Layout and Production by David Lane Published by and Copyright 2002 by The Royal Astronomical Society of Canada 136 Dupont Street Toronto, Ontario, M5R 1V2 Canada www.rasc.ca — [email protected] Table of Contents Preface ....................................................................................2 Volume Number Reference ...................................................3 Subject Index Reference ........................................................4 Subject Index ..........................................................................7 Author Index ..................................................................... 121 Abstracts of Papers Presented at Annual Meetings of the National Committee for Canada of the I.A.U. (1967–1970) and Canadian Astronomical Society (1971–1996) .......................................................................168 Abstracts of Papers Presented at the Annual General Assembly of the Royal Astronomical Society of Canada (1969–1996) ...........................................................207 JRASC Index (1967-1996) Page 1 PREFACE The last cumulative Index to the Journal, published in 1971, was compiled by Ruth J. Northcott and assembled for publication by Helen Sawyer Hogg. It included all articles published in the Journal during the interval 1932–1966, Volumes 26–60. In the intervening years the Journal has undergone a variety of changes. In 1970 the National Newsletter was published along with the Journal, being bound with the regular pages of the Journal. In 1978 the National Newsletter was physically separated but still included with the Journal, and in 1989 it became simply the Newsletter/Bulletin and in 1991 the Bulletin. That continued until the eventual merger of the two publications into the new Journal in 1997. -
Moore Et Al., 1977
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E2, PAGES 3413-3429, FEBRUARY 25, 1993 SOIL TEXTURE AND GRANULOMETRY AT THE SURFACE OF MARS Audouin Dollfus and Marc Deschamps Observatoire de Paris, Meudon, France James R. Zimbelman Center for Earth and Planetary Sciences, National Air and Space Museum Smithsonian Institution, Washington, D. C. The physical behavior of the Martian surface soil has been characterized remotely by both photopolarimetry and radiometry. The degree of linear polarization defines a coefficient b which is related to the top surface soil texture and is calibrated in terms of grain size, or as a fraction of the area exhibiting uncovered clean rocks. This coefficient b was recorded with the instrument VPM (Visual Polarimeter Mars) on board Soviet orbiter MARS 5 in 1974. The radiometric thermal inertia coefficient I is essentially a measurement of the soil compaction, or an effective average particle size in the soil texture, through the few decimeters below the top surface sensed by polarimetry. The instrument IBTM (Infra Bed Thermal Mapper) was used on board the Viking spacecraft between 1976 and 1982. The polarimetric scans raked a strip covering two contrasting regions, the dark-hued Mare Erythraeum and the light-hued Thaumasia. Over these wide areas, several smaller typical terrains were characterized by the three parameters A (albedo), b (related to top surface grain size) and I (underlaying compaction or block size). The large dark region Erythraeum is characterized everywhere by a uniform polarization response, despite the large geomorphological diversity of the surface. The values of A and b indicate a ubiquitous coating or mantling with small dark grains of albedo 12.7%, with a radius of 10 to 20 urn.