1 / 26

Structure of Atmosphere

Structure of Atmosphere. From Cunningham & Cunningham, 2004, Fig. 9.1. Wavelength and energy. What are the 3 ways heat can be transferred?. Radiation : transfer by electromagnetic waves. Conduction : transfer by molecular collisions. Convection : transfer by circulation of a fluid.

nora
Télécharger la présentation

Structure of Atmosphere

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Structure of Atmosphere From Cunningham & Cunningham, 2004, Fig. 9.1

  2. Wavelength and energy

  3. What are the 3 ways heat can be transferred? • Radiation: transfer by electromagnetic waves. • Conduction: transfer by molecular collisions. • Convection: transfer by circulation of a fluid. Image from: http://www.uwsp.edu/geo/faculty/ritter/geog101/uwsp_lectures/ lecture_radiation_energy_concepts.html#Radiation

  4. Sun - our star – the source of most of our energy For the entire earth, climate can be explained by: 1) the amount of sunlight received and 2) the character of the surface receiving it.

  5. Reflected = 25 + 5 = 30 Absorbed = 25 + 45 = 70 Energy Balance From Cunningham & Cunningham, 2004, Fig. 9.2

  6. Sun’s energy is emitted in the form of electromagnetic radiation (Radiant Energy) • Radiant energy can interact with matter in 3 ways. • Most often its behavior is a combination of two or more of these modes • Reflection - there is no change in the matter because of the radiant energy that strikes it and it does not let the energy pass through it (i.e. it is opaque to the radiant energy), then it reflects the energy. Reflection only changes the direction of the beam of radiant energy, not its wavelength or amplitude. • Transparent - matter allows radiant energy to pass through it unchanged. Again, there is no change in any of the properties of the radiant energy. • Absorption –energy is transferred from the radiant beam to the matter resulting in an increase in molecular energy of the matter, later released as infared radiation

  7. Reflectivity = Albedo • Reflected Energy/ Incident Energy • Higher reflectivity = brighter, shinier surface (snow, ice) • Lower reflectivity = darker, rougher surface (soil, sand) • Water – depends on the angle of the sun • Average albedo for Earth = 30 • Average albedo for moon = 7 Image from: http://www.fourmilab.ch/earthview/vplanet.html

  8. Energy Balance Incoming = 45 +88 = 133 Outgoing = 104 + 24 + 5 = 133 From Cunningham & Cunningham, 2004, Fig. 9.2

  9. Latent heat of fusion & vaporization Heat energy released 540 cal/gm 80 cal/gm

  10. How much heat is released ? • Text book calculation • 1 inch (= 2.54 cm) of rain • 1 km square area • 580 cal/cm3 (540 + 40 deg.) • 2.54 cm/ 1 in * 100,000 cm/ km * 100,000 cm/km * 580 cal/ cm3 = 17.2 x 1011 calories

  11. Greenhouse Effect Hot Earth - Cartoon

  12. Radiation - and wavelength • Energy may be transferred from one object to another without the space between them being heated. (This is the mechanism where earth receives energy from the sun as radiation. ) • Waves of radiation can be distinguished by wavelength, which is the distance between two successive crests of the wave.

  13. Wavelength and energy

  14. Radiation - and wavelength. This is the Key to the Greenhouse Effect • The solar radiation reaching earth is in three wavelength spectra. • The sun emits 41% of its radiation in the visible spectrum, • 9% in the ultraviolet spectrum (short wave), and • 50% in the infrared spectrum (long wave). Image from: http://www.uwsp.edu/geo/faculty/ritter/geog101/uwsp_lectures/lecture_radiation_energy_concepts.html#Radiation

  15. Radiation Laws - Black Body Radiation • Several physical laws describe the properties of electromagnetic radiation that is emitted by a perfect radiator, a so-called black body. • By definition, at a given temperature, a black bodyabsorbs all radiation incident on it at every wavelength and emits all radiation at every wavelength at the maximum rate possible for a given temperature; • No radiation is reflected. • A blackbody is therefore a perfect absorber and a perfect emitter.

  16. Radiation Laws - Black Body Radiation • The term black body can be misleading because the concept does not refer to color. • Objects that do not appear black may none the less be be blackbodies, perfect radiators. • Most gases are not blackbodies • Both the Sun and the Earth closely approximate perfect radiators, so that we can apply blackbody radiation laws to them. • We'll discuss 2, • ) Wien's displacement law and the • 2) Stefan-Boltzmann law.

  17. Radiation Laws - Wien's Displacement Law • Although all known objects emit all forms of electromagnetic radiation, the wavelength of most intense radiation is inversely proportional to the T. ( 1/T) • Implications: • Sun emits @ ~ 6000 deg Kelvin • Earth emits @ 278 deg Kelvin, • Which will emit radiation at the longer wavelength? • Earth • The peak of Solar output is in the visible (light, shorter) part of the electromagnetic spectrum while the Earth, emits most of its energy in the infrared (heat, longer) portion of the electromagnetic spectrum

  18. Radiation Laws - Wien's displacement law • What does this mean in terms of the Earth and the Sun? • Warm objects, Sun (6000°K) emit peak radiation at relatively short wavelengths (0.5 micrometers ( 1 millionth of a meter) = yellow-green visible) • Colder objects Earth-atmosphere (average T of 278 °K, 15°C, 59°F) emit peak radiation at longer wavelengths ( 10 microns – infrared part of the spectrum) • Most of the sun's energy is emitted in a spectrum from 0.15 µm to 4 µm. 41% of it is visible, 9% is uv, 50 % infra-red. • Earths radiant energy, stretches from 4 m to 100µm, with maximum energy falling at about 10.1 µm (infrared).

  19. Radiation Laws - Stefan-Boltzmann law • Would you expect the same amount of electromagnetic radiation to be emitted by the Earth and Sun? • No. The total energy radiated by an object is proportional to the fourth power of it's absolute T • F = k (T4) = Stefan-Boltzmann law. • F (rate of energy emitted) • k = Stefan-Boatman constant ( 5.67 x 10-8 Wm-2 K-4) • Sun radiates at a much higher temperature than Earth.- • Sun’s energy output/m2 = 160,000 that of Earth

  20. Comparison -Earth & Sun Radiation • Sun – more energy & shorter wavelength • Earth-lower energy and longer wavelength

  21. Atmospheric Composition % by Volume Major Constituents Nitrogen 78.1 Oxygen 20.9 Active Minor Constituents Water vapor (H2O) variable (0.48 aver.) Carbon Dioxide (CO2) 0.035 Methane (CH4) 0.00014 Nitrous oxide (NO2) 0.00005 Ozone (O3) 0.000007 CFC’s 0.00000014 H2O (liq & ice) 0.00000002 Inactive Minor Constituents Argon 0.93 Neon 0.0018 Helium 0.00052 Krypton 0.0001 Xenon 0.000009

  22. Greenhouse Gases – Why are they a problem?

  23. What are some of the Greenhouse Gases? • Water Vapor • Molecular Ozone Antrhopogenic increases of these: • CO2 • Methane • Nitrous Oxide • CFCs • Know the contribution of gases marked in green,to the greenhouse effect, where they come from, rates of increase

  24. Mauna Loa Observatory CO2 Measurements • 50-60% of greenhouse effect • ~0.5% increase /year • CO2 in atmosphere today ~370 ppm • Estimated pre-industrial concentration -= 288 ppm • Highest past level that we can measure in ice cores, ~125,000 years ago (280-300 ppm!)

  25. Greenhouse Effect Hot Earth - Cartoon

  26. Heat Budget Extra version of Energy Balance Heat Budget

More Related