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Saturn — from the Outside In
Saturn — From the Outside In Saturn — From the Outside In Questions, Answers, and Cool Things to Think About Discovering Saturn:The Real Lord of the Rings Saturn — From the Outside In Although no one has ever traveled ing from Saturn’s interior. As gases in from Saturn’s atmosphere to its core, Saturn’s interior warm up, they rise scientists do have an understanding until they reach a level where the tem- of what’s there, based on their knowl- perature is cold enough to freeze them edge of natural forces, chemistry, and into particles of solid ice. Icy ammonia mathematical models. If you were able forms the outermost layer of clouds, to go deep into Saturn, here’s what you which look yellow because ammonia re- trapped in the ammonia ice particles, First, you would enter Saturn’s up- add shades of brown and other col- per atmosphere, which has super-fast ors to the clouds. Methane and water winds. In fact, winds near Saturn’s freeze at higher temperatures, so they equator (the fat middle) can reach turn to ice farther down, below the am- speeds of 1,100 miles per hour. That is monia clouds. Hydrogen and helium rise almost four times as fast as the fast- even higher than the ammonia without est hurricane winds on Earth! These freezing at all. They remain gases above winds get their energy from heat ris- the cloud tops. Saturn — From the Outside In Warm gases are continually rising in Earth’s Layers Saturn’s atmosphere, while icy particles are continually falling back down to the lower depths, where they warm up, turn to gas and rise again. -
ESSENTIALS of METEOROLOGY (7Th Ed.) GLOSSARY
ESSENTIALS OF METEOROLOGY (7th ed.) GLOSSARY Chapter 1 Aerosols Tiny suspended solid particles (dust, smoke, etc.) or liquid droplets that enter the atmosphere from either natural or human (anthropogenic) sources, such as the burning of fossil fuels. Sulfur-containing fossil fuels, such as coal, produce sulfate aerosols. Air density The ratio of the mass of a substance to the volume occupied by it. Air density is usually expressed as g/cm3 or kg/m3. Also See Density. Air pressure The pressure exerted by the mass of air above a given point, usually expressed in millibars (mb), inches of (atmospheric mercury (Hg) or in hectopascals (hPa). pressure) Atmosphere The envelope of gases that surround a planet and are held to it by the planet's gravitational attraction. The earth's atmosphere is mainly nitrogen and oxygen. Carbon dioxide (CO2) A colorless, odorless gas whose concentration is about 0.039 percent (390 ppm) in a volume of air near sea level. It is a selective absorber of infrared radiation and, consequently, it is important in the earth's atmospheric greenhouse effect. Solid CO2 is called dry ice. Climate The accumulation of daily and seasonal weather events over a long period of time. Front The transition zone between two distinct air masses. Hurricane A tropical cyclone having winds in excess of 64 knots (74 mi/hr). Ionosphere An electrified region of the upper atmosphere where fairly large concentrations of ions and free electrons exist. Lapse rate The rate at which an atmospheric variable (usually temperature) decreases with height. (See Environmental lapse rate.) Mesosphere The atmospheric layer between the stratosphere and the thermosphere. -
Cloud and Precipitation Radars
Sponsored by the U.S. Department of Energy Office of Science, the Atmospheric Radiation Measurement (ARM) Climate Research Facility maintains heavily ARM Radar Data instrumented fixed and mobile field sites that measure clouds, aerosols, Radar data is inherently complex. ARM radars are developed, operated, and overseen by engineers, scientists, radiation, and precipitation. data analysts, and technicians to ensure common goals of quality, characterization, calibration, data Data from these sites are used by availability, and utility of radars. scientists to improve the computer models that simulate Earth’s climate system. Storage Process Data Post- Data Cloud and Management processing Products Precipitation Radars Mentors Mentors Cloud systems vary with climatic regimes, and observational DQO Translators Data capabilities must account for these differences. Radars are DMF Developers archive Site scientist DMF the only means to obtain both quantitative and qualitative observations of clouds over a large area. At each ARM fixed and mobile site, millimeter and centimeter wavelength radars are used to obtain observations Calibration Configuration of the horizontal and vertical distributions of clouds, as well Scan strategy as the retrieval of geophysical variables to characterize cloud Site operations properties. This unprecedented assortment of 32 radars Radar End provides a unique capability for high-resolution delineation Mentors science users of cloud evolution, morphology, and characteristics. One-of-a-Kind Radar Network Advanced Data Products and Tools All ARM radars, with the exception of three, are equipped with dual- Reectivity (dBz) • Active Remotely Sensed Cloud Locations (ARSCL) – combines data from active remote sensors with polarization technology. Combined -60 -40 -20 0 20 40 50 60 radar observations to produce an objective determination of hydrometeor height distributions and retrieval with multiple frequencies, this 1 μm 10 μm 100 μm 1 mm 1 cm 10 cm 10-3 10-2 10-1 100 101 102 of cloud properties. -
The Sun's Dynamic Atmosphere
Lecture 16 The Sun’s Dynamic Atmosphere Jiong Qiu, MSU Physics Department Guiding Questions 1. What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere cool off farther away from the Sun’s center? 2. What intrinsic properties of the Sun are reflected in the photospheric observations of limb darkening and granulation? 3. What are major observational signatures in the dynamic chromosphere? 4. What might cause the heating of the upper atmosphere? Can Sound waves heat the upper atmosphere of the Sun? 5. Where does the solar wind come from? 15.1 Introduction The Sun’s atmosphere is composed of three major layers, the photosphere, chromosphere, and corona. The different layers have different temperatures, densities, and distinctive features, and are observed at different wavelengths. Structure of the Sun 15.2 Photosphere The photosphere is the thin (~500 km) bottom layer in the Sun’s atmosphere, where the atmosphere is optically thin, so that photons make their way out and travel unimpeded. Ex.1: the mean free path of photons in the photosphere and the radiative zone. The photosphere is seen in visible light continuum (so- called white light). Observable features on the photosphere include: • Limb darkening: from the disk center to the limb, the brightness fades. • Sun spots: dark areas of magnetic field concentration in low-mid latitudes. • Granulation: convection cells appearing as light patches divided by dark boundaries. Q: does the full moon exhibit limb darkening? Limb Darkening: limb darkening phenomenon indicates that temperature decreases with altitude in the photosphere. Modeling the limb darkening profile tells us the structure of the stellar atmosphere. -
The Cloud Cycle and Acid Rain
gX^\[`i\Zk\em`ifed\ekXc`dgXZkjf]d`e`e^Xkc`_`i_`^_jZ_ffcYffbc\k(+ ( K_\Zcfl[ZpZc\Xe[XZ`[iX`e m the mine ke fro smo uld rain on Lihir? Co e acid caus /P 5IJTCPPLMFUXJMM FYQMBJOXIZ K_\i\Xjfe]fik_`jYffbc\k K_\i\`jefXZ`[iX`efeC`_`i% `jk_Xkk_\i\_XjY\\ejfd\ K_`jYffbc\k\ogcX`ejk_\jZ`\eZ\ d`jle[\ijkXe[`e^XYflkk_\ Xe[Z_\d`jkipY\_`e[XZ`[iX`e% \o`jk\eZ\f]XZ`[iX`efeC`_`i% I\X[fekfÔe[flkn_pk_\i\`jef XZ`[iX`efeC`_`i55 page Normal rain cycle and acid rain To understand why there is no acid rain on Lihir we will look at: 1 How normal rain is formed 2 2 How humidity effects rain formation 3 3 What causes acid rain? 4 4 How much smoke pollution makes acid rain? 5 5 Comparing pollution on Lihir with Sydney and China 6 6 Where acid rain does occur 8–9 7 Could acid rain fall on Lihir? 10–11 8 The effect of acid rain on the environment 12 9 Time to check what you’ve learnt 13 Glossary back page Read the smaller text in the blue bar at the bottom of each page if you want to understand the detailed scientific explanations. > > gX^\) ( ?fnefidXciX`e`j]fid\[ K_\eXkliXcnXk\iZpZc\ :cfl[jXi\]fid\[n_\e_\Xk]ifdk_\jleZXlj\jk_\nXk\i`e k_\fZ\Xekf\mXgfiXk\Xe[Y\Zfd\Xe`em`j`Yc\^Xj% K_`j^Xji`j\j_`^_`ekfk_\X`in_\i\Zffc\ik\dg\iXkli\jZXlj\ `kkfZfe[\ej\Xe[Y\Zfd\k`epnXk\i[ifgc\kj%N_\edXepf] k_\j\nXk\i[ifgc\kjZfcc`[\kf^\k_\ik_\pdXb\Y`^^\inXk\i [ifgj#n_`Z_Xi\kff_\XmpkfÕfXkXifle[`ek_\X`iXe[jfk_\p ]Xcc[fneXjiX`e%K_`jgifZ\jj`jZXcc\[gi\Z`g`kXk`fe% K_\eXkliXcnXk\iZpZc\ _\Xk]ifd k_\jle nXk\imXgflijZfe[\ej\ kfZi\Xk\Zcfl[j gi\Z`g`kXk`fe \mXgfiXk`fe K_\jZ`\eZ\Y\_`e[iX`e K_\_\Xk]ifdk_\jleZXlj\jnXk\i`ek_\ -
The Atmosphere!
Activity 1 What’s Up? The Atmosphere! Atmosphere CHANGE IS IN THE AIR Forces of Change » Atmosphere » Activity 1 » Page 1 ACTIVITY 1 What’s Up? The Atmosphere! In one of 80 experiments performed on the space shuttle Columbia before its tragic loss during reentry in 2003, Israeli astronaut Ilan Ramon tracked desert dust in the atmosphere as it moved around the earth Photo © Ernest Hilsenrath. Overview Students learn the distinctions of each layer of the atmosphere and sketch the layers. Suggested Grade Level 6–8 National Standards National Science Education Standards Alignment Earth and Science Standard, Content Standard D: Grades 5–8 Structure of the Earth System: The atmosphere is a mixture of nitrogen, oxygen, and trace gases that include water vapor. The atmosphere has different properties at different elevations. Time One class period (40–50 minutes) Materials 1 Graph paper 1 Activity sheet Forces of Change » Atmosphere » Activity 1 » Page 2 ACTIVITY 1 OBJECTIVES Students will be able to: e Describe the main layers of Earth’s atmosphere, the proportion of each in the atmosphere, and what role each plays in atmospheric phenomena. r Define how the temperature varies from layer to layer of atmosphere. t Calculate the quantities of gases in a particular volume of air, such as their classroom. Background What we call the atmosphere comes in five main layers: exosphere, thermosphere, mesosphere, stratosphere, and troposphere. In the exosphere (640 to 64,000 km, or 400 to 40,000 mi), air dwin- dles to nothing as molecules drift into space. The thermosphere (80 to 640 km or 50 to 400 mi) is very hot despite being very thin because it The Aura Earth-observing satellite absorbs so much solar radiation. -
Jupiter and Saturn
Jupiter and Saturn 1 2 3 Guiding Questions 1. Why is the best month to see Jupiter different from one year to the next? 2. Why are there important differences between the atmospheres of Jupiter and Saturn? 3. What is going on in Jupiter’s Great Red Spot? 4. What is the nature of the multicolored clouds of Jupiter and Saturn? 5. What does the chemical composition of Jupiter’s atmosphere imply about the planet’s origin? 6. How do astronomers know about the deep interiors of Jupiter and Saturn? 7. How do Jupiter and Saturn generate their intense magnetic fields? 8. Why would it be dangerous for humans to visit certain parts of the space around Jupiter? 9. How was it discovered that Saturn has rings? 10.Are Saturn’s rings actually solid bands that encircle the planet? 11. How uniform and smooth are Saturn’s rings? 4 12.How do Saturn’s satellites affect the character of its rings? Jupiter and Saturn are the most massive planets in the solar system • Jupiter and Saturn are both much larger than Earth • Each is composed of 71% hydrogen, 24% helium, and 5% all other elements by mass • Both planets have a higher percentage of heavy elements than does the Sun • Jupiter and Saturn both rotate so rapidly that the planets are noticeably flattened 5 Unlike the terrestrial planets, Jupiter and Saturn exhibit differential rotation 6 Atmospheres • The visible “surfaces” of Jupiter and Saturn are actually the tops of their clouds • The rapid rotation of the planets twists the clouds into dark belts and light zones that run parallel to the equator • The -
Nitrogen Dioxide Pollution As a Signature of Extraterrestrial Technology
Draft version February 10, 2021 Typeset using LATEX default style in AASTeX63 Nitrogen Dioxide Pollution as a Signature of Extraterrestrial Technology Ravi Kopparapu ,1 Giada Arney,1 Jacob Haqq-Misra ,2 Jacob Lustig-Yaeger ,3 and Geronimo Villanueva 1 1NASA Goddard Space Flight Center 8800 Greenbelt Road Greenbelt, MD 20771, USA 2Blue Marble Space Institute of Science, Seattle, WA, USA 3Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA Submitted to ApJ ABSTRACT Nitrogen dioxide (NO2) on Earth today has biogenic and anthropogenic sources. During the COVID- 19 pandemic, observations of global NO2 emissions have shown significant decrease in urban areas. Drawing upon this example of NO2 as an industrial byproduct, we use a one-dimensional photo- chemical model and synthetic spectral generator to assess the detectability of NO2 as an atmospheric technosignature on exoplanets. We consider cases of an Earth-like planet around Sun-like, K-dwarf and M-dwarf stars. We find that NO2 concentrations increase on planets around cooler stars due to less short-wavelength photons that can photolyze NO2. In cloud-free results, present Earth-level NO2 on an Earth-like planet around a Sun-like star at 10pc can be detected with SNR ∼ 5 within ∼ 400 hours with a 15 meter LUVOIR-like telescope when observed in the 0:2 − 0:7µm range where NO2 has a strong absorption. However, clouds and aerosols can reduce the detectability and could mimic the NO2 feature. Historically, global NO2 levels were 3x higher, indicating the capability of detecting a 40-year old Earth-level civilization. Transit and direct imaging observations to detect infrared spectral signatures of NO2 on habitable planets around M-dwarfs would need several 100s of hours of obser- vation time, both due to weaker NO2 absorption in this region, and also because of masking features by dominant H2O and CO2 bands in the infrared part of the spectrum. -
Cold Season Cloud Seeding
Weather Modification UNDERSTANDING Cloud seeding—a form of weather modification— ALBERTA CANADA COLD SEASON is a safe, scientific, time-tested, and proven set of Cloud Seeding technologies used to enhance rain and snow, re- ND duce hail damage, and alleviate fog. The benefits ID of cloud seeding can be measured in additional WY water for cities and agriculture, as well as the re- NV UT duction of damage from severe weather. CA CO KS TX Target area—Cold-season cloud-seeding Target area—Warm-season cloud-seeding A ground-based generator is used to burn a silver iodide solution to release microscopic silver-iodide particles which can create additional ice crystals, then snow, in winter clouds. Research has shown that placing equipment at high elevations increases cloud seeding effectiveness. NAWMC Members Cold Season Seeding California Department of Water Resources When moist air flows over the mountains, water vapor Colorado Water Conservation Board condenses and forms clouds composed of water droplets. These droplets become “super cooled” and have the unique Desert Research Institute quality to remain liquid even at temperatures below freez- North Dakota Atmospheric Resource Board ing. Given enough time and mixing with surrounding air, many of the droplets will evaporate, but under the correct Texas Department of Licensing and Regulation conditions some will eventually become ice crystals, grow Utah Division of Water Resources into snowflakes and precipitate to the ground. Cloud seed- Wyoming Water Development Office ing provides an opportunity to increase the number of ice crystals that can become snowflakes. NAWMC Associate Members Who Conducts Cloud Seeding? Central Arizona Water Conservation District In North America, cloud-seeding programs are conducted in Metropolitan Water District of Southern California California, Colorado, Idaho, Nevada, Utah, Wyoming, Kansas, Santa Barbara County Water Agency North Dakota, and Texas, as well as Alberta, Canada. -
Morphology and Dynamics of the Venus Atmosphere at the Cloud Top Level As Observed by the Venus Monitoring Camera
Morphology and dynamics of the Venus atmosphere at the cloud top level as observed by the Venus Monitoring Camera Von der Fakultät für Elektrotechnik, Informationstechnik, Physik der Technischen Universität Carolo-Wilhelmina zu Braunschweig zur Erlangung des Grades eines Doktors der Naturwissenschaften (Dr.rer.nat.) genehmigte Dissertation von Richard Moissl aus Grünstadt Bibliografische Information Der Deutschen Bibliothek Die Deutsche Bibliothek verzeichnet diese Publikation in der Deutschen Nationalbibliografie; detaillierte bibliografische Daten sind im Internet über http://dnb.ddb.de abrufbar. 1. Referentin oder Referent: Prof. Dr. Jürgen Blum 2. Referentin oder Referent: Dr. Horst-Uwe Keller eingereicht am: 24. April 2008 mündliche Prüfung (Disputation) am: 9. Juli 2008 ISBN 978-3-936586-86-2 Copernicus Publications, Katlenburg-Lindau Druck: Schaltungsdienst Lange, Berlin Printed in Germany Contents Summary 7 1 Introduction 9 1.1 Historical observations of Venus . .9 1.2 The atmosphere and climate of Venus . .9 1.2.1 Basic composition and structure of the Venus atmosphere . .9 1.2.2 The clouds of Venus . 11 1.2.3 Atmospheric dynamics at the cloud level . 12 1.3 Venus Express . 16 1.4 Goals and structure of the thesis . 19 2 The Venus Monitoring Camera experiment 21 2.1 Scientific objectives of the VMC in the context of this thesis . 21 2.1.1 UV Channel . 21 2.1.1.1 Morphology of the unknown UV absorber . 21 2.1.1.2 Atmospheric dynamics of the cloud tops . 21 2.1.2 The two IR channels . 22 2.1.2.1 Water vapor abundance and cloud opacity . 22 2.1.2.2 Surface and lower atmosphere . -
Lecture 7A: Cloud Development and Forms
Lecture 7a: Cloud Development and Forms (from “The Blue Planet”) Why Clouds Form Cloud Types ESS55 Prof. Jin-Yi Yu Why Clouds Form? Clouds form when air rises and becomes saturated in response to adiabatic cooling. ESS55 Prof. Jin-Yi Yu Four Ways to Lift Air Upward (1) Localized Convection cold front (2) Convergence (4) Frontal Lifting Lifting warm front (3) Orographic Lifting ESS55 (from “The Blue Planet”) Prof. Jin-Yi Yu Orographic Lifting ESS55 Prof. Jin-Yi Yu Frontal Lifting When boundaries between air of unlike temperatures (fronts) migrate, warmer air is pushed aloft. This results in adiabatic cooling and cloud formation. Cold fronts occur when warm air is displaced by cooler air. Warm fronts occur when warm air rises over and displaces cold air. ESS55 Prof. Jin-Yi Yu Cloud Type Based On Properties Four basic cloud categories: Cirrus --- thin, wispy cloud of ice. Stratus --- layered cloud Cumulus --- clouds having vertical development. Nimbus --- rain-producing cloud These basic cloud types can be combined to generate ten different cloud types, such as cirrostratus clouds that have the characteristics of cirrus clouds and stratus clouds. ESS55 Prof. Jin-Yi Yu Cloud Types ESS55 Prof. Jin-Yi Yu Cloud Types Based On Height If based on cloud base height, the ten principal cloud types can then grouped into four cloud types: High clouds -- cirrus, cirrostratus, cirroscumulus. Middle clouds – altostratus and altocumulus Low clouds – stratus, stratocumulus, and nimbostartus Clouds with extensive vertical development – cumulus and cumulonimbus. (from “The Blue Planet”) ESS55 Prof. Jin-Yi Yu Cloud Classifications (from “The Blue Planet”) ESS55 Prof. -
Titan Fact Sheet Titan Is a Large Moon Orbiting the Planet Saturn, About
Titan Fact Sheet Titan is a large moon orbiting the planet Saturn, about 866 million miles from the sun. The surface of Titan is hidden by the thick, hazy atmosphere, but in the past few years spacecraft have managed to collect images and other data that tell us about what lies beneath the haze. They found something that’s common on Earth but very unusual in the rest of the solar system: lakes and seas! Besides Earth, Titan is the only body in our solar system with enough liquid on its surface to fill lakes and seas. Titan’s lakes and seas are filled mainly with thick tar-like substances, such as methane and ethane. Titan also has methane gas in its atmosphere, just as Earth has water vapor in its atmosphere. Titan has summer and winter seasons when its surface becomes warmer and colder. However, because it is so far from the sun, even in summer Titan is very cold. Its average surface temperature is about -179 degrees Celsius or -290 degrees Fahrenheit. Titan Fact Sheet Titan is a large moon orbiting the planet Saturn, about 866 million miles from the sun. The surface of Titan is hidden by the thick, hazy atmosphere, but in the past few years spacecraft have managed to collect images and other data that tell us about what lies beneath the haze. They found something that’s common on Earth but very unusual in the rest of the solar system: lakes and seas! Besides Earth, Titan is the only body in our solar system with enough liquid on its surface to fill lakes and seas.