Appendix I Glossary
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E-Region Auroral Ionosphere Model
atmosphere Article AIM-E: E-Region Auroral Ionosphere Model Vera Nikolaeva 1,* , Evgeny Gordeev 2 , Tima Sergienko 3, Ludmila Makarova 1 and Andrey Kotikov 4 1 Arctic and Antarctic Research Institute, 199397 Saint Petersburg, Russia; [email protected] 2 Earth’s Physics Department, Saint Petersburg State University, 199034 Saint Petersburg, Russia; [email protected] 3 Swedish Institute of Space Physics, 981 28 Kiruna, Sweden; [email protected] 4 Saint Petersburg Branch of Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of Russian Academy of Sciences (IZMIRAN), 199034 Saint Petersburg, Russia; [email protected] * Correspondence: [email protected] Abstract: The auroral oval is the high-latitude region of the ionosphere characterized by strong vari- ability of its chemical composition due to precipitation of energetic particles from the magnetosphere. The complex nature of magnetospheric processes cause a wide range of dynamic variations in the auroral zone, which are difficult to forecast. Knowledge of electron concentrations in this highly turbulent region is of particular importance because it determines the propagation conditions for the radio waves. In this work we introduce the numerical model of the auroral E-region, which evaluates density variations of the 10 ionospheric species and 39 reactions initiated by both the solar extreme UV radiation and the magnetospheric electron precipitation. The chemical reaction rates differ in more than ten orders of magnitude, resulting in the high stiffness of the ordinary differential equations system considered, which was solved using the high-performance Gear method. The AIM-E model allowed us to calculate the concentration of the neutrals NO, N(4S), and N(2D), ions + + + + + 4 + 2 + 2 N ,N2 , NO ,O2 ,O ( S), O ( D), and O ( P), and electrons Ne, in the whole auroral zone in the Citation: Nikolaeva, V.; Gordeev, E.; 90-150 km altitude range in real time. -
Aeronomy and Astrophysics
Aeronomy and astrophysics A southern high-latitude geomagnetic index: AES-80 C.G. MACLENNAN, Bell Laboratories, Lucent Technologies, Murray Hill, New Jersey 07974 P. B ALLATORE, Istito de Fisica della Spazio Interplanetario, Consiglio Nazionale della Ricerche, c.p. 27, 00044 Frascati, Rome, Italy M.J. ENGEBRETSON, Department of Physics, Augsburg College, Minneapolis, Minnesota 55454 L.J. LANZEROTTI, Bell Laboratories, Lucent Technologies, Murray Hill, New Jersey 07974 eomagnetic measurements obtained at McMurdo Sta- G tion (Arrival Heights) and at two of the U.S. automatic geophysical observatories (AGO-1; AGO-4) are being com- bined with measurements made at Casey and Dumont D'Urville to construct a Southern Hemisphere geomagnetic index for the geomagnetic latitude 80°S. The calculation of the index is modeled on the calculation of the Northern Hemi- sphere auroral electrojet index AE and is thus called the AES- 80 index. The AE index was developed to monitor geomagnetic activity at auroral zone latitudes in the Northern Hemisphere (Davis and Sugiura 1966) and indicates the level of auroral electrojet currents and in particular the occurrence of sub- storms (Baumjohann 1986). It is calculated as the difference between the upper (AU) and the lower (AL) envelope of mag- netograms from 12 observatories located at northern geomag- netic latitudes between 60° and 70° and rather uniformly distributed over all longitudes. Because of the land mass dis- tribution in Antarctica, it is impossible to have ground obser- vatories located uniformly at geomagnetic latitudes between 60° and 70°S (see figure 1). Unlike in the Northern Hemisphere, Figure 1. Map of Antarctica, with the stations used to calculate the however, it is possible in Antarctica to have reasonable ground AES-80 index shown as filled circles. -
UPPER ATMOSPHERE RESEARCH at INPE B.R. Clbmesha Department of Geophysics and Aeronomy Instituto De Pesquisas Espaciais
UPPER ATMOSPHERE RESEARCH AT INPE B.R. CLbMESHA Department of Geophysics and Aeronomy Instituto de Pesquisas Espaciais - INPE ABSTRACT Upper atmosphere research at INPE is mainly concerned with the chemistry and dynamics of the stratosphere, upper mesosphere and lower thermosphere, and the middle thermo- sphere. Experimental work includes lidar observations of the stratospheric aerosol, measurements of stratospheric ozone by Dobson spectrophotometers and by balloon and rocket-borne sondes, lidar measurements of atmospheric sodium, and photom- etric observations of 0, 02 , OH and Na emissions, including interferometric measurements of the 016300 emission for the purpose of determining thermospheric winds and temperature. The airglow observations also include measurements of a number of emissions produced by the precipitation of ener- getic neutral particles generated by charge exchange in the ring current. Some recent results of INPE's upper atmosphere program are presented.ii» this paper. ' ' n/ .71. 1- INTRODUCTION INPK maintains an active program of research into a number of aspects of upper atmosphere science, including both experimental and theoretical studies of the dynamics and chemistry of the stratosphere, mesosphere and lower thermosphere. Hxperimental work involves mainly ground-based optical techniques, although balloon and rocket-borne sondes are used for studies of stratospheric ozone, and a rocket-borne photometer payload is under development for measurements of a number of emissions from the thermosphere. Theoretical studies include numerical model- ling with special reference to a number of minor constituents related to the experimental measurements. In the following sec- tions we present a brief description of INPE's experimental fa- cilities in the area of upper atmosphere science, and outline some recent results. -
Status of NSF Space Physics
Status of NSF Space Physics Rich Behnke Therese Moretto, Bob Robinson, Anja Stromme, and Ray Walker National Academy – March 7,2013 • Status and Updates • NSF Response to the Academy’s “Solar and Space Physics: A Science for a Technological Society 2 The Five Geospace Programs • Solar Physics -- Paul Bellaire has retired, new PD has been selected – but not signed. • Magnetospheric Physics – Ray Walker • Aeronomy – Anja Stromme • Geospace Facilities – Bob Robinson • Space Weather and Instrumentation -- Therese Moretto Aeronomy (AER) • Typically around 95 proposals per year, about 1/3 funded. Budget is about $11M • Home of CEDAR • Program Director --Anja Stromme (SRII) 4 Magnetospheric Physics (MAG) • typically around 90 proposals per year, 1/3 funded. Budget is about $8.5M. • Home of GEM • Program Director – Ray Walker (UCLA) 5 Solar Physics Program (STR) •Typically around 80 proposals per year, 1/3 funded. Budget is about $8.5M •Home of SHINE •Program Director – Paul Bellaire/TBA 6 The Geospace Facilities Program (GS) Program Director – Bob Robinson • Six incoherent scatter radar sites (five awards:~$12M) • Lidar Consortium (six institutions: ~$1M) • Miscellaneous facility-related awards (facility supplements, CAREER, REU, Workshops, schools: ~1M) SuperDARN is being expanded • The Mid-latitude SuperDARN Array ( AGS’s first midscale project): New SuperDARN radars have been constructed and are operational at: Fort Hays, Kansas; Christmas Valley, Oregon; and Adak, Alaska • Negotiations are underway with Portuguese officials in the Azores -
Lecture 35. Stratospheric Ozone Chemistry. 1. the Formation of Ozone
Lecture 35. Stratospheric ozone chemistry. Part 1. Formation and destruction of stratospheric ozone. Objectives: 1. The formation of ozone: Chapman mechanism. 2. Catalytic ozone destruction. 3. Ozone and UV radiation. Readings: Turco: p. 407-414; Brimblecombe: 190-194. 1. The formation of ozone: Chapman mechanism. “Bad ozone”: in photochemical smog -> health threat in the troposphere -> contributes to global warming “Good ozone”: in the stratosphere -> absorbs biologically harmful UV radiation emitted by sun. Most of the Earth’s atmosphere ozone (about 90%) is found in the stratosphere. Typical ozone concentrations: in very clean troposphere: 10 – 40 ppb; in ozone layer at 25-30 km: about 10 ppm; • The ozone column abundance is typically specified in Dobson units. One Dobson unit, DU, is the thickness that the ozone column would occupy at standard temperature and pressure (T =273.2 K, P = 1 atm): 1 DU = 10-3 atm cm =2.69x1016 molecules cm-2 Total column ozone values range from about 290 to 310 DU over the globe. 1 In 1930 S.Chapman, a British scientist, proposed a theory of the formation of ozone in the stratosphere (known as Chapman mechanism): Major steps of Chapman mechanism: 1) Above about 30 km altitude, molecular oxygen absorbs solar radiation (wavelength < 242 nm) and photodissociates: O2 + hν -> O + O 2) The oxygen atom, O, reacts rapidly with O2 in the presence of a third body, denoted M (M is usually another O2 or N2), to form ozone: O2 + O + M -> O3 + M NOTE: above reaction is the only reaction that produces ozone in the atmosphere!!! 3) Ozone absorbs solar radiation (in the wavelength range of 240 to 320 nm) and decomposes back to O2 and O: O3 + hν -> O2 + O 4) Additionally, ozone can react with atomic oxygen to regenerate two molecules of O2: O3 + O -> O2 + O2 2 Let’s consider the dynamic behavior of reactions (1) –(4). -
The Distribution of Ozone and Ozone-Depleting Substances in the Atmosphere and Observed Changes
THE DISTRIBUTION OF OZONE AND OZONE-DEPLETING SUBSTANCES IN THE ATMOSPHERE AND OBSERVED CHANGES 1.1 GLOBAL OZONE MEASUREMENT (see Chapter 3). Intrusions of stratospheric air are also a signif- AND MONITORING icant source of ozone in the troposphere (see Chapter 2). Globally, the distribution and climatology of tropospheric Ozone (O3), an allotrope of ordinary oxygen (O2), is the most important trace constituent in the stratosphere. Although it is ozone appear to be highly variable and have not yet been present in relative concentrations of no more than a few parts well established by comprehensive measurements. Although per million, it is such an efficient absorber of ultraviolet radia- this is a very important area of current research, this docu- tion that it is the largest source of heat in the atmosphere at ment will deal primarily with the state of current knowledge altitudes between about 10 and 50 km. UV absorption by of ozone in the stratosphere. ozone causes the temperature inversion that is responsible for Regular measurments of the ozone content of the atmos- the existence of the stratosphere. Ozone is also an important phere were initiated in the early 1920s by G.M.B. Dobson radiator, with strong emission bands in the 9.6 mm infrared using spectrographic instruments. He built his first version of region. In the UV-B region (290–315 nm) it absorbs with an what is now known as the Dobson ozone spectrophotometer efficiency that increases exponentially with decreasing wave- in 1927. It makes precise measurements of the relative intensi- length, and so strongly that at 290 nm the radiation at the ties of sunlight at pairs of wavelengths in the UV spectrum; 1 ground is reduced by more than a factor of 104 from that the total ozone column is deduced from these measurements above the ozone layer (see Chapter 4). -
CEDAR an Aeronomy Initiative
Eos, Vol. 68, No. 2, January 13, 1987 Rep. 4, Bur. Gravimetrique Int., Toulouse, data, terrestrial gravity and other data, Rep. Bernard Moynot re France, 1982. 322, Dep. of Geodetic Sci. and Surveying, ceived his degree in mathe Balmino, G., C. Brossier, A. Cazenave, and F. Ohio State Univ., Columbus, 1982. matics from the Ecole Nor Nouel, Geoid of the Kerguelen Islands area Rapp, R. H., The determination of geoid un male Superieure of Paris determined from GEOS 3 Altimeter data, dulations and gravity anomalies from Sea in 1963. In 1956, he be /. Geophys. Res., 84, 3827, 1979. sat altimeter data,/ Geophys. Res., 88, 1552, gan working with the Cen Cazenave, A., B. Lago, and K. Dominh, 1983a. tre National d'Etudes Spa Thermal parameters of the oceanic litho- Rapp, R. H., The development of the Janu tiales, performing research sphere estimated from geoid height data, J. ary 1983 1° x 1° mean free-air anomaly in satellite geodesy and nu Geophys. Res., 88, 1105, 1983. data tape, internal report, Dept. of Geodet merical analysis. He is now Haxby, W. F., G. D. Karner, J. F. Labrecque, ic Sci. and Surveying, Ohio State Univ., Co with the Bureau Gravime and J. K. Weissel, Digital images of com lumbus, 1983ft. trique International in Toulouse. bined oceanic and continental data sets and Reigber, C, H. Muller, W. Bosch, G. Bal Michel Sarrailh gradu their use in tectonic studies, Eos Trans. mino, and B. Moynot, GRIM gravity model ated from the Institut de AGU, 64, 995, 1983. improvement using LAGEOS (GRIM 3- Physique du Globe in Lazarewicz, A. -
Chapter 10 Chapter 10 – Ozone Holes
Environmental Transport and Fate Chapter 10 – Ozone Holes Benoit Cushman-Roisin Thayer School of Engineering Dartmouth College Recall the vertical structure of the atmosphere We are now concerned about this lithlayer in the middle of the stratosphere 1 Temperature increases in this layer of the atmosphere because of absorption of solar radiation by oxygen and ozone. Photochemical reactions are: O2 + (UV radiation < 242 nm) → O● + O● O● + O2 + M → O3 + M● (M stands for any molecule nearby) O3 + (UV-C or UV-B radiation) → O2 + O● O2 absorption < 242 nm O3 absorption 200 nm < < 320 nm 2 Cartoon from Cartoon US EPA 3 Example of what is happening on the seasonal scale of ozone Where was the stratospheric ozone by the end of the winter? And, it did get worse for a number of years… 1 DU = 1 Dobson Unit = thickness of O3 brought to 1 atm @ 0oC (in meters) x 105 Historical springtime vertically integrated ozone over Halley Bay, Antarctica (76oS) (Source: UNEP, 1994) 4 Historical data showing no minimum in spring sphere/winter_bulletins/sh_07/ o Pronounced minimum in springs from mid- 1980s to present. www.cpc.noaa.gov/products/strat / http:/ Hole still occurring in 2010 and 2011 The Antarctic Ozone Hole The Antarctic Ozone Hole was discovered by the British Antarctic Survey from data obtained with a ground-based instrument at a measuring station located in Halley Bay, Antarctica, in the 1981-1983 period. A first report of October ozone loss was issued in 1985. Satellite measurements then confirmed edtattesp that the springt gteooeossasacotime ozone loss was a contin etent-wide featu r e. -
PRL, Ahmedabad ATMOSPHERIC PHYSICS
PRL, Ahmedabad ATMOSPHERIC PHYSICS Books 1 BRASSEUR G AERONOMY OF THE MIDDLE ATMOSPHERE: CHEMISTRY AND PHYSICS OF THE STRATOSPHERE AND MESOSPHERE (UN COURSE). 551.510.5 BRA. B16453 2 BRASSEUR G AERONOMY OF THE MIDDLE ATMOSPHERE: CHEMISTRY AND PHYSICS OF THE STRATOSPHERE AND MESOSPHERE (UN COURSE). 551.510.5 BRA. B16666 3 BRASSEUR G AERONOMY OF THE MIDDLE ATMOSPHERE: CHEMISTRY AND PHYSICS OF THE STRATOSPHERE AND MESOSPHERE (UN COURSE). 551.510.5 BRA. B16664 4 BRASSEUR G AERONOMY OF THE MIDDLE ATMOSPHERE: CHEMISTRY AND PHYSICS OF THE STRATOSPHERE AND MESOSPHERE (UN COURSE). 551.510.5 BRA. B16665 5 BRASSEUR G AERONOMY OF THE MIDDLE ATMOSPHERE: CHEMISTRY AND PHYSICS OF THE STRATOSPHERE AND MESOSPHERE (UN COURSE). 551.510.5 BRA. B16663 6 GARRATT JR ATMOSPHERIC BOUNDARY LAYER. 551.510.5 GAR. B18859 7 GREEN J ATMOSPHERIC DYNAMICS (UN COURSE). 55.51 GRE. B16654 8 GREEN J ATMOSPHERIC DYNAMICS (UN COURSE). 551.51 GRE. B16621 9 GREEN J ATMOSPHERIC DYNAMICS (UN COURSE). 551.51 GRE. B16631 10 GREEN J ATMOSPHERIC DYNAMICS (UN COURSE). 551.51 GRE. B16669 11 IRIBARNE JV ATMOSPHERIC PHYSICS. 551.510.5 IRI. B11738 12 BURGER JJ ED ATMOSPHERIC PHYSICS FROM SPACELAB PROCEEDINGS OF THE 11TH ESLAB SYMPOSIUM HELD AT FRASCATI, ITALY IN 1976 (ASTROPHYS & SPACE SCI LIB V 61). 551.507.3(063) BUR. B8044 13 SISKIND DE ED ATMOSPHERIC SCIENCE ACROSS THE STRATOPAUSE. 551.51 SIS. B17271 14 KYLE TG ATMOSPHERIC TRANSMISSION EMISSION & SCATTERING. 551.51 KYL. B14788 15 HOBBS PV BASIC PHYSICAL CHEMISTRY FOR THE ATMOSPHERIC SCIENCES : A COMPANATIONAL INSTITUTE OF OCEANOGRAPHYN TEXT TO "INTRODUCTION TO ATMOSPHERIC CHEMISTRY". -
Careers in Atm Scien. Factsheet
Fact ����� National Aeronautics and Space Administration ������� �������� ������ Hampton, Virginia 23681-2199 FS-2002-12-65-LaRC Choosing a Career in Atmospheric Science Atmospheric science is the study of the physics and 2. Data analysis and modeling — the examination of chemistry of clouds, gases, and aerosols (airborne the data produced by the experiments and the particles) that surround the planetary bodies of development of theoretical models to interpret the the solar system. Research in atmospheric science data. The result is an improvement of our under- includes such varied areas of interest as: standing of atmospheric motions and chemistry, climate change, and weather forecasting. This area • Climatology — the study of long-term weather and requires experience in computer science, temperature trends mathematics, chemistry, physics, meteorology, • Dynamic meteorology — the study of the motions radiative transfer, or fluid dynamics. of the atmosphere • Meteorology —the study of weather and climate. 3. Laboratory studies — the examination of • Cloud physics — the formation and evolution of the chemical and physical processes that occur clouds and precipitation in the atmosphere, including cloud microphysics, • Atmospheric chemistry — the chemical photochemical reactions, and absorption and composition of the atmosphere emission of radiation by atmospheric gases and • Atmospheric physics — the study of processes particles. This area requires experience in such as heating and cooling of the atmosphere quantitative laboratory techniques, chemistry, or • Aeronomy — the study of the upper atmosphere spectroscopy. • Oceanography — the study of the Earthʼs oceans and how they affect the atmosphere The majority of atmospheric scientists in the United States work for the Federal Government. The largest Most atmospheric scientists study the atmosphere of number of civilian atmospheric scientists work for the the Earth, while others study the atmospheres of the National Weather Service and other branches of the planets and moons in our solar system. -
Global Change and Sustainability
FOLE_C18FF.QXD 9/10/08 6:39 PM Page 268 EXERCISE 18 Global Change and Sustainability INTRODUCTION doubters are funded by special interest groups and fossil fuel coalitions that do not want research on, or “The public in the industrialized nations, particularly in evidence of, global change that could impact their the United States, must be made more aware of the economic condition (Gelbspan, 1997). Island nations, pervasive trends in environmental degradation and environmentalists, active geoscientists, environmen- resource depletion, and of the need to modify pat- tal economists, and insurance organizations were terns of life to cope with these trends.” among the first to recognize that global change is —KAULA AND ANDERSON, PLANET EARTH COMMITTEE, occurring. Now many groups are working on adapta- AMERICAN GEOPHYSICAL UNION, 1991 tions to change and on ways to reduce human “The time to consider the policy dimensions of cli- impact globally. mate change is not when the link between green- We should be able to adapt to the limits of our house gases and climate change is conclusively habitat on Earth without overshooting them. Many proven Á but when the possibility cannot be dis- organisms undergo increases and collapses in their counted and is taken seriously by the society of populations but they do not have our technology, which we are part. We in BP have reached that information, and understanding. We have models, point.” examples, and explanations of why societies collapse (Diamond, 2005). We probably will never understand —JOHN BROWNE, GROUP CHIEF EXECUTIVE, how the total Earth system works; however, we need BP AMERICA, 1997 to write the “Operating Manual for Spaceship Earth.” The quotations above capture the concern of many The final activity in this exercise is constructing a geologists who understand Earth history and scenario—your description of the future viewed from change in the Earth system. -
(AECC-2) in Environmental Studies Semester-2
Ability Enhancement Compulsory Course-2 (AECC-2) in Environmental Studies Semester-2 Total Marks - 100 (Credit -2) (50 Theory-MCQ type + 30 Project + 10 Internal Assessment + 10 Attendance ) Unit 6: Environmental Policies & Practices Unit 6: Environmental Policies & Practices • Climate Change : We know that the Climate is average of weather over time across large regions. On the other hand the Weather is what is happening in one small region at one time. The global climate always changes, and there are many reasons for that, such as the interactions between components in the climate system like oceans, atmosphere, etc. The cyclone Aila was actually a climatic phenomenon, where the change in surface temperature over the Indian ocean formed the tropical cyclone Aila over the Bay of Bengal on May 23, 2009, causing extensive damage in India and Bangladesh. The climate change occurs because when the amount of energy in the entire climate system is changed it affects each and every component in the system. We the humans are also responsible for the climate change. Human activities like the burning of fossil fuel increases the amount of carbon dioxide (CO 2) and other greenhouse gases in the atmosphere, enhancing the natural greenhouse effect. Increasing CO 2 causes the planet to heat up. The concentration of atmospheric CO 2 has increased by at least 40% in the last 200 years. The last time CO 2 increased this much was over a period of 6000 years, when the earth came out of an ice age, and the average surface temperature rose by 5 oC. Burning fossil fuels, changes in land use (such as deforestation), small particles like smoke and dust in the atmosphere (aerosols) have altered the amount of sunlight that can reflected back into space.