DOCSLIB.ORG

The Meteorology of Jupiter the Visible Features of the Giant Planet Reflect the Circulation of Its Atmosphere

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Meteorology of Jupiter the Visible Features of the Giant Planet Reflect the Circulation of Its Atmosphere The Meteorology of Jupiter The visible features of the giant planet reflect the circulation of its atmosphere. A model reproducing those features should apply to other planetary atmospheres, including the earth's by Andrew P. Ingersoll very feature that is visible in a picture mospheres of the two planets consist chiefly inferred ratio of helium to hydrogen in the of the planet Jupiter is a cloud: the of noncondensable gases: hydrogen and he­ sun (I 15). It is the abundance ratios, to­ E : dark belts, the light-colored zones lium on Jupiter, nitrogen and oxygen on the gether with the low density of Jupiter as a and the Great Red Spot. The solid surface, earth; mixed in are small amounts of water whole, that suggest that the planet is very if indeed there is one, lies many thousands vapor and other gases that do condense, much like the sun in its composition. of kilometers below the visible surface. Yet forming clouds. In terms of the temperature The amount of heat Jupiter radiates im­ most of the atmospheric features of Jupiter changes that would occur on the two plan­ plies that the interior of the planet is hot. If have an extremely long lifetime and an or­ ets if the condensable vapors were entirely it were cold, there would not be enough ganized structure that is unknown in atmo­ converted into liquid or solid form, thus heat in the interior to have lasted until the spheric features of the earth. Those differ­ releasing all their latent heat, Jupiter's at­ present time. A consequence of the hot-in­ ences, and the fact that atmospheric fea­ mosphere would be somewhat less affected terior model of Jupiter is that solids cannot tures are easy to observe on Jupiter, make by condensation than the earth's. Clouds, form in it. According to current thinking, the giant planet a laboratory where terres­ condensation and precipitation are none­ the planet is mostly liquid, with a gradual trial meteorologists can test theories about theless important in the dynamics of both transition to a gaseous atmosphere in the atmospheric dynamics in ways not possible atmospheres. outermost few thousand kilometers. on the earth. Spectroscopic data at infrared and radio Jupiter's diameter is 11 times larger than ur picture of the average composition wavelengths also yield information about the earth's; its surface gravity is 2.4 times O and vertical structure of the Jovian the temperature and pressure in the Jovian stronger; it rotates on its axis 2.4 times fast­ atmosphere is based partly on observation atmosphere. At the deepest levels the tem­ er (once every 10 hours). There is little or no and partly on theory. Spectroscopic studies perature decreases with altitude at the rate change of season on Jupiter because the axis from the earth have established that the of some two degrees Celsius per kilometer. of the planet's rotation is nearly parallel to atmosphere is mostly molecular hydrogen That rate is close to the adiabatic lapse rate, the axis of its orbit around the sun. (Hz), with smaller amounts of methane which is the value of the temperature gradi­ Jupiter's atmosphere and interior are (CH4), ammonia (NH3) and a growing list ent in a well-mixed atmosphere. In such an mostly hydrogen, with other elements such of other gases. In those studies absorption adiabatic atmosphere parcels of gas move as helium, carbon, oxygen and nitrogen features in the infrared spectrum of Jupiter vertically without exchanging heat with mixed with the hydrogen in the same pro­ are compared with absorption features in neighboring parcels. They get cooler or portions as they are in the sun. Because that the spectrum of gases in the laboratory. warmer, but they do so only because their mixture does not solidify at the tempera­ Since each gas has characteristic wave­ pressure changes as they ascend or descend. tures and pressures that have been calculat­ lengths at which it absorbs radiation, ab­ Neighboring parcels at the same level in the ed to exist on Jupiter, the planet is probably sorption spectra of the Jovian atmosphere atmosphere are indistinguisliable from one gaseous or liquid throughout its interior. make it possible to positively identify most another. An adiabatic temperature gradient The mixture is gently stirred at all depths by of the gases in it even in very small concen­ also usually implies that the atmosphere is convection currents that carry heat from trations. The exception is helium, which ab­ stirred by convection. the interior to the surface. Theoretical cal­ sorbs radiation only in the ultraviolet region The temperature in Jupiter's atmosphere culations indicate that the internal heat is of the spectrum at wavelengths that can­ is 165 degrees Kelvin (degrees C. above ab­ most likely left over from Jupiter's initial not be observed through the earth's atmo­ solute zero) at the level where the pressure gravitational contraction, when it con­ sphere. Helium was recently detected, how­ is one atmosphere (the pressure of the densed out of the nebula that also gave rise ever, by an ultraviolet spectrometer on the earth's atmosphere at sea level). The tem­ to the sun and the other planets. The spacecraft Pioneer 10, and the effect of the perature continues to decrease with height amount of internal energy Jupiter releases helium on the infrared spectra of other gas­ until it reaches a minimum value of 105 at present is approximately equal to the es in the Jovian atmosphere has also been degrees K. at the level where the pressure is amount of energy it absorbs from the sun. observed. .1 atmosphere. At that point it begins to rise From the point of view of meteorology From the relative strengths of the absorp­ slightly once again. By analogy with the the most important differences between Ju­ tion spectra of hydrogen, methane and am­ earth's atmosphere this minimum marks piter and the earth lie in the fact that Jupiter monia the relative abundances of those gas­ the beginning of the Jovian stratosphere. In has an appreciable internal energy source es can be determined. On Jupiter the ratio that layer of the Jovian atmosphere the tem­ and probably lacks a solid surface. The oth­ of the number of carbon atoms to hydro­ perature is controlled largely by radiation er differences-in radius, gravity, rate of ro­ gen atoms is about 1 : 3,000 and the ratio rather than by convection. tation and so on-are mainly differences of of nitrogen atoms to hydrogen atoms is There are thin clouds on Jupiter as high degree. Even the chemical composition of I : 10,000. Those abundances are close to as the base of the stratosphere. Broken thick Jupiter's atmosphere is similar to the chem­ the abundances of the same elements in the clouds, with holes opening into deeper lev­ ical composition of the earth's as far as its sun. Within wide limits the ratio of helium els, begin to be present where the pressure is effect on meteorology is concerned. The at- to hydrogen in Jupiter is consistent with the between .6 and one atmosphere. The pres- 46 © 1976 SCIENTIFIC AMERICAN, INC sure at the cloud tops on Jupiter is thus height above an arbitrary base level. His University of Arizona detected water on Ju­ similar to the pressure at the cloud tops on calculations show that the deepest and piter for the first time by observing radia­ the earth. The temperatures at those levels thickest clouds are condensed water, since tion that emerged through holes in the up­ on Jupiter are much lower, however, since both oxygen and hydrogen are abundant per cloud layers from water molecules at Jupiter is five times farther from the sun in the atmosphere. Above those clouds deeper levels. than the earth is. are clouds of ammonium hydrosulfide Lewis' model, which assumes that all the (NH4SH) and above those in turn are substances are at chemical equilibrium at he composition of the Jovian cloud par­ clouds of pure ammonia (NH3)' The level of each level, cannot account for the colors of Tticles and the nature of the material that each cloud depends on the vapor pressure of the clouds. The cloud particles in that mod­ endows them with their remarkable colors the particular condensate, which is a strong el are white, whereas the Jovian clouds are cannot be determined from spectroscopy function of temperature. The less volatile subtle shades of red, brown, white and blue. alone. Here theoretical calculations by John substances such as water condense at higher With convection bringing up exotic materi­ S. Lewis of the Massachusetts Institute of temperatures (deeper in the atmosphere) al from deeper levels, however, and with Technology have been useful. Lewis began than the more volatile substances such as ultraviolet radiation from the sun energiz­ by assuming that Jupiter's atmosphere has ammonia. The relatively low vapor pressure ing chemical reactions at the top of the at­ the same composition as the sun's at the of water at the temperatures characteristic mosphere, it is not surprising that portions ranges of temperature and pressure ob­ of the Jovian cloud tops also explains why of Jupiter's atmosphere do depart from served on the planet, and that all its constit­ water vapor was found there only recently: local chemical equilibrium. Only small uents are at chemical equilibrium. He then water cannot be detected spectroscopically amounts of coloring material are needed calculated the amount of solid and liquid unless it is in the form of a vapor. In 1974 to explain the observations, and an atmo­ matter in the atmosphere as a function of Harold P.
Load more

Recommended publications
  • Cornell University Ithaca, New York 14650 JOSE - JUPITER ORBITING SPACECRAFT
    N T Z 33854 C *?** IS81 1? JOSE - JUPITER ORBITING SPACECRAFT: A SYSTEMS STUDY Volume I '>•*,' T COLLEGE OF ENGINEERING Cornell University Ithaca, New York 14650 JOSE - JUPITER ORBITING SPACECRAFT: A SYSTEMS STUDY Volume I Prepared Under Contract No. NGR 33-010-071 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION by NASA-Cornell Doctoral Design Trainee Group (196T-TO) October 1971 College of Engineering Cornell University Ithaca, New York Table of Contents Volume I Preface Chapter I: The Planet Jupiter: A Brief Summary B 1-2 r. Mechanical Properties of the Planet Jupiter. P . T-fi r> 1-10 F T-lfi F T-lfi 0 1-29 H, 1-32 T 1-39 References ... p. I-k2 Chapter II: The Spacecraft Design and Mission Definition A. Introduction p. II-l B. Organizational Structure and the JOSE Mission p. II-l C. JOSE Components p. II-1* D. Proposed Configuration p. II-5 Bibliography and References p. 11-10 Chapter III: Mission Trajectories A. Interplanetary Trajectory Analysis .... p. III-l B. Jupiter Orbital Considerations p. III-6 Bibliography and References. p. 111-38 Chapter IV: Attitude Control A. Introduction and Summary . p. IV-1 B. Expected Disturbance Moments M in Interplanetary Space . p. IV-3 C. Radiation-Produced Impulse Results p. IV-12 D. Meteoroid-Produced Impulse Results p. IV-13 E. Inertia Wheel Analysis p. IV-15 F. Attitude System Tradeoff Analysis p. IV-19 G. Conclusion P. IV-21 References and Bibliography p. TV-26 Chapter V: Propulsion Subsystem A. Mission Requirements p. V-l B. Orbit Insertion Analysis p.
    [Show full text]
  • Stratosphere-Troposphere Coupling: a Method to Diagnose Sources of Annular Mode Timescales
    STRATOSPHERE-TROPOSPHERE COUPLING: A METHOD TO DIAGNOSE SOURCES OF ANNULAR MODE TIMESCALES Lawrence Mudryklevel, Paul Kushner p R ! ! SPARC DynVar level, Z(x,p,t)=− T (x,p,t)d ln p , (4) g !ps x,t p ( ) R ! ! Z(x,p,t)=− T (x,p,t)d ln p , (4) where p is the pressure at the surface, R is the specific gas constant and g is the gravitational acceleration s g !ps(x,t) where p is the pressure at theat surface, the surface.R is the specific gas constant and g is the gravitational acceleration Abstract s Geopotentiallevel, Height Decomposition Separation of AM Timescales p R ! ! at the surface. This time-varying geopotentialZ( canx,p,t be)= decomposed− T into(x,p a,t cli)dmatologyln p , and anomalies from the(4) climatology AM timescales track seasonal variations in the AM index’s decorrelation time6,7. For a hydrostatic fluid, geopotential height may be describedg !p sas(x ,ta) function of time, pressure level Timescales derived from Annular Mode (AM) variability provide dynamical and ashorizontalZ(x,p,t position)=Z (asx,p a )+temperatureδZ(x,p,t integral). Decomposing from the Earth’s the temperature surface to a andgiven surface pressure pressure fields inananalogous insight into stratosphere-troposphere coupling and are linked to the strengthThis of time-varying level, geopotentialwhere can beps is decomposed the pressure at into the a surface, climatologyR is the and specific anomalies gas constant from and theg is climatology the gravitational acceleration NCEP, 1958-2007 level: ^ a) o (yL ) d) o AM responses to climate forcings.
    [Show full text]
  • Lecture 23: Jupiter Solar System Jupiter's Orbit
    Lecture 23: Jupiter Solar System Jupiter’s Orbit •The semi-major axis of Jupiter’s orbit is a = 5.2 AU Jupiter Sun a •Kepler’s third law relates the semi-major axis to the orbital period 1 Jupiter’s Orbit •Kepler’s third law relates the semi-major axis a to the orbital period P 2 3 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years⎠ ⎝ AU ⎠ •Solving for the period P yields 3/ 2 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years ⎠ ⎝ AU ⎠ •Since a = 5.2 AU for Jupiter, we obtain P = 11.9 Earth years •Jupiter’s orbit has eccentricity e = 0.048 Jupiter’s Orbit •The distance from the Sun varies by about 10% during an orbit Dperihelion = 4.95 AU Daphelion = 5.45 AU •Like Mars, Jupiter is easiest to observe during favorable opposition •At this time, the Earth-Jupiter distance is only about 3.95 AU Earth Jupiter Jupiter Sun (perihelion) (aphelion) •Jupiter appears full during favorable opposition Bulk Properties of Jupiter •Jupiter is the largest planet in the solar system •We have for the radius and mass of Jupiter Rjupiter = 71,400 km = 11.2 Rearth 30 Mjupiter = 1.9 x 10 g = 318 Mearth •The volume of Jupiter is therefore given by 4 V = π R 3 jupiter 3 jupiter 30 3 •Hence Vjupiter = 1.5 x 10 cm 2 Bulk Properties of Jupiter •The average density of Jupiter is therefore M × 30 ρ = jupiter = 1.9 10 g jupiter × 30 3 Vjupiter 1.5 10 cm •We obtain ρ = −3 jupiter 1.24 g cm •This is much less than the average density of the Earth •Hence there is little if any iron and no dense core inside Jupiter Bulk Properties of Jupiter •The average density of the Earth is equal to −3 ρ⊕ = 6 g cm •The density
    [Show full text]
  • Adaptive Multibody Gravity Assist Tours Design in Jovian System for the Ganymede Landing
    TO THE ADAPTIVE MULTIBODY GRAVITY ASSIST TOURS DESIGN IN JOVIAN SYSTEM FOR THE GANYMEDE LANDING Grushevskii A.V.(1), Golubev Yu.F.(2), Koryanov V.V.(3), and Tuchin A.G.(4) (1)KIAM (Keldysh Institute of Applied Mathematics), Miusskaya sq., 4, Moscow, 125047, Russia, +7 495 333 8067, E-mail: [email protected] (2)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] (3)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] (4)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] Keywords: gravity assist, adaptive mission design, trajectory design, TID, phase beam Introduction Modern space missions inside Jovian system are not possible without multiple gravity assists (as well as in Saturnian system, etc.). The orbit design for real upcoming very complicated missions by NASA, ESA, RSA should be adaptive to mission parameters, such as: the time of Jovian system arrival, incomplete information about ephemeris of Galilean Moons and their gravitational fields, errors of flybys implementation, instrumentation deflections. Limited dynamic capabilities, taking place in case of maneuvering around Jupiter's moons, demand multiple encounters (about 15-30 times) for these purposes. Flexible algorithm of current mission scenarios synthesis (specially selected) and their operative transformation is required. Mission design is complicated due to requirements of the Ganymede Orbit Insertion (GOI) ("JUICE" ESA) and also Ganymede Landing implementation ("Laplas-P" RSA [1]) comparing to the ordinary early ―velocity gain" missions since ―Pioneers‖ and "Voyagers‖. Thus such scenario splits in two parts. Part 1(P1), as usually, would be used to reduce the spacecraft’s orbital energy with respect to Jupiter and set up the conditions for more frequent flybys.
    [Show full text]
  • Our Planetary System (Chapter 7) Based on Chapter 7
    Our Planetary System (Chapter 7) Based on Chapter 7 • This material will be useful for understanding Chapters 8, 9, 10, 11, and 12 on “Formation of the solar system”, “Planetary geology”, “Planetary atmospheres”, “Jovian planet systems”, and “Remnants of ice and rock” • Chapters 3 and 6 on “The orbits of the planets” and “Telescopes” will be useful for understanding this chapter Goals for Learning • How do planets rotate on their axes and orbit the Sun? • What are the planets made of? • What other classes of objects are there in the solar system? Orbits mostly lie in the same flat plane All planets go around the Sun in the same direction Most orbits are close to circular Not coincidences! Most planets rotate in the same “sense” as they orbit the Sun Coincidence? Planetary equators mostly lie in the same plane as their orbits Coincidence? • Interactive Figure: Orbital and Rotational Properties of the Planets Rotation and Orbits of Moons • Most moons (especially the larger ones) orbit in near-circular orbits in the same plane as the equator of their parent planet • Most moons rotate so that their equator is in the plane of their orbit • Most moons rotate in the same “sense” as their orbit around the parent planet • Everything is rotating/orbiting in the same direction A Brief Tour • Distance from Sun •Size •Mass • Composition • Temperature • Rings/Moons Sun 695000 km = 108 RE 333000 MEarth 98% Hydrogen and helium 99.9% total mass of solar system Surface = 5800K Much hotter inside Giant ball of gas Gravity => orbits Heat/light => weather
    [Show full text]
  • Jupiter Mass
    CESAR Science Case Jupiter Mass Calculating a planet’s mass from the motion of its moons Student’s Guide Mass of Jupiter 2 CESAR Science Case Table of Contents The Mass of Jupiter ........................................................................... ¡Error! Marcador no definido. Kepler’s Three Laws ...................................................................................................................................... 4 Activity 1: Properties of the Galilean Moons ................................................................................................. 6 Activity 2: Calculate the period of your favourite moon ................................................................................. 9 Activity 3: Calculate the orbital radius of your favourite moon .................................................................... 12 Activity 4: Calculate the Mass of Jupiter ..................................................................................................... 15 Additional Activity: Predict a Transit ............................................................................................................ 16 To know more… .......................................................................................................................... 19 Links ............................................................................................................................................ 19 Mass of Jupiter 3 CESAR Science Case Background Kepler’s Three Laws The three Kepler’s Laws, published between
    [Show full text]
  • The Effect of Jupiter\'S Mass Growth on Satellite Capture
    A&A 414, 727–734 (2004) Astronomy DOI: 10.1051/0004-6361:20031645 & c ESO 2004 Astrophysics The effect of Jupiter’s mass growth on satellite capture Retrograde case E. Vieira Neto1;?,O.C.Winter1, and T. Yokoyama2 1 Grupo de Dinˆamica Orbital & Planetologia, UNESP, CP 205 CEP 12.516-410 Guaratinguet´a, SP, Brazil e-mail: [email protected] 2 Universidade Estadual Paulista, IGCE, DEMAC, CP 178 CEP 13.500-970 Rio Claro, SP, Brazil e-mail: [email protected] Received 13 June 2003 / Accepted 12 September 2003 Abstract. Gravitational capture can be used to explain the existence of the irregular satellites of giants planets. However, it is only the first step since the gravitational capture is temporary. Therefore, some kind of non-conservative effect is necessary to to turn the temporary capture into a permanent one. In the present work we study the effects of Jupiter mass growth for the permanent capture of retrograde satellites. An analysis of the zero velocity curves at the Lagrangian point L1 indicates that mass accretion provides an increase of the confinement region (delimited by the zero velocity curve, where particles cannot escape from the planet) favoring permanent captures. Adopting the restricted three-body problem, Sun-Jupiter-Particle, we performed numerical simulations backward in time considering the decrease of M . We considered initial conditions of the particles to be retrograde, at pericenter, in the region 100 R a 400 R and 0 e 0:5. The results give Jupiter’s mass at the X moment when the particle escapes from the planet.
    [Show full text]
  • Thermal Structure and Composition of Jupiter's Great Red Spot from High-Resolution Thermal Imaging
    Thermal Structure and Composition of Jupiter’s Great Red Spot from High-Resolution Thermal Imaging Leigh N. Fletchera,b, G. S. Ortona, O. Mousisc,d, P. Yanamandra-Fishera, P. D. Parrishe,a, P. G. J. Irwinb, B. M. Fishera, L. Vanzif, T. Fujiyoshig, T. Fuseg, A.A. Simon-Millerh, E. Edkinsi, T.L. Haywardj, J. De Buizerk aJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA bAtmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK cInstitut UTINAM, CNRS-UMR 6213, Observatoire de Besan¸con, Universit´ede Franche-Comt´e, Besan¸con, France dLunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA eSchool of GeoScience, University of Edinburgh, Crew Building, King’s Buildings, Edinburgh, EH9 3JN, UK fPontificia Universidad Catolica de Chile, Department of Electrical Engineering, Av. Vicuna Makenna 4860, Santiago, Chile. gSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 650 North A’ohoku Place, Hilo, Hawaii 96720, USA hNASA/Goddard Spaceflight Center, Greenbelt, Maryland, 20771, USA iUniversity of California, Santa Barbara, Santa Barbara, CA 93106, USA jGemini Observatory, Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile. kSOFIA - USRA, NASA Ames Research Center, Moffet Field, CA 94035, USA. Abstract Thermal-IR imaging from space-borne and ground-based observatories was used to investigate the temperature, composition and aerosol structure of Jupiter’s Great Red Spot (GRS) and its temporal variability between 1995-2008. An elliptical warm core, extending over 8◦ of longitude and 3◦ of latitude, was observed within the cold anticyclonic vortex at 21◦S.
    [Show full text]
  • 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.
    [Show full text]
  • On the Impact of Future Climate Change on Tropopause Folds and Tropospheric Ozone
    https://doi.org/10.5194/acp-2019-508 Preprint. Discussion started: 14 June 2019 c Author(s) 2019. CC BY 4.0 License. On the impact of future climate change on tropopause folds and tropospheric ozone Dimitris Akritidis1, Andrea Pozzer2, and Prodromos Zanis1 1Department of Meteorology and Climatology, School of Geology, Aristotle University of Thessaloniki, Thessaloniki, Greece 2Max Planck Institute for Chemistry, Mainz, Germany Correspondence: D. Akritidis ([email protected]) Abstract. Using a transient simulation for the period 1960-2100 with the state-of-the-art ECHAM5/MESSy Atmospheric Chemistry (EMAC) global model and a tropopause fold identification algorithm, we explore the future projected changes in tropopause folds, Stratosphere-to-Troposphere Transport (STT) of ozone and tropospheric ozone under the RCP6.0 scenario. Statistically significant changes in tropopause fold frequencies are identified in both Hemispheres, occasionally exceeding 3%, 5 which are associated with the projected changes in the position and intensity of the subtropical jet streams. A strengthen- ing of ozone STT is projected for future at both Hemispheres, with an induced increase of transported stratospheric ozone tracer throughout the whole troposphere, reaching up to 10 nmol/mol in the upper troposphere, 8 nmol/mol in the middle troposphere and 3 nmol/mol near the surface. Notably, the regions exhibiting the maxima changes of ozone STT at 400 hPa, coincide with that of the highest fold frequencies, highlighting the role of tropopause folding mechanism in STT process under 10 a changing climate. For both the eastern Mediterranean and Middle East (EMME), and the Afghanistan (AFG) regions, which are known as hotspots of fold activity and ozone STT during the summer period, the year-to-year variability of middle tropo- spheric ozone with stratospheric origin is largely explained by the short-term variations of ozone at 150 hPa and tropopause folds frequency.
    [Show full text]
  • 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.
    [Show full text]
  • Cold Plasma Diagnostics in the Jovian System
    341 COLD PLASMA DIAGNOSTICS IN THE JOVIAN SYSTEM: BRIEF SCIENTIFIC CASE AND INSTRUMENTATION OVERVIEW J.-E. Wahlund(1), L. G. Blomberg(2), M. Morooka(1), M. André(1), A.I. Eriksson(1), J.A. Cumnock(2,3), G.T. Marklund(2), P.-A. Lindqvist(2) (1)Swedish Institute of Space Physics, SE-751 21 Uppsala, Sweden, E-mail: [email protected], [email protected], mats.andré@irfu.se, [email protected] (2)Alfvén Laboratory, Royal Institute of Technology, SE-100 44 Stockholm, Sweden, E-mail: [email protected], [email protected], [email protected], per- [email protected] (3)also at Center for Space Sciences, University of Texas at Dallas, U.S.A. ABSTRACT times for their atmospheres are of the order of a few The Jovian magnetosphere equatorial region is filled days at most. These atmospheres can therefore rightly with cold dense plasma that in a broad sense co-rotate with its magnetic field. The volcanic moon Io, which be termed exospheres, and their corresponding ionized expels sodium, sulphur and oxygen containing species, parts can be termed exo-ionospheres. dominates as a source for this cold plasma. The three Observations indicate that the exospheres of the three icy Galilean moons (Callisto, Ganymede, and Europa) icy Galilean moons (Europa, Ganymede and Callisto) also contribute with water group and oxygen ions. are oxygen rich [1, 2]. Several authors have also All the Galilean moons have thin atmospheres with modelled these exospheres [3, 4, 5], and the oxygen was residence times of a few days at most.
    [Show full text]