1. 6061 Geoscience Systems (http://vortex.ihrc.fiu.edu/GSS6061/GSS6061.htm) Atmospheric Radiation Energy Budget How the atmosphere system is driven? Lecture 1

2. The Changing Seasons Are Due to the Tilt of Earth’s Axis Earth-Sun relationship

4. Length of daylight

7. Transport by atmospheric motion and ocean currents Net transport by atmosphere and ocean Transient motion Ocean currents Atmospheric motions

8. Forms of Energy Kinetic energy: Energy associated with motion. Potential energy: Energy stored within a physical system. It has the potential to be converted into other forms of energy, such as kinetic energy, and to do work in the process. Heat (symbolized by Q): energy transferred from one body or system to another due to a difference in temperature. Mechanisms of Energy Transfer 1. Conduction: transfer of heat through electron and molecule collisions. 2. Convection: heat transfer that involves motion or circulation.

9. 3. Radiation: in the form of electromagnetic waves

10. Solar radiation Electromagnetic Radiation

11. 2. Wien’s displacement law 300K 6000K Laws of blackbody radiation 1. Plank’s law Gray body:

12. Selective absorption and emission of atmospheric gases 1. Energy level of atoms or molecules Quantum jump: transition between different energy levels 2. Different energy form of a molecule or atom What Happens to Incoming Solar Radiation

13. a. Rotational energy CO Rotational energy transition can happen as long as a photon’s wavelength is shorter than 1 cm, usually associated with microwave wavelength. b. Vibrational energy Polar molecule has permanent dipole Non-polar molecule does not have permanent dipole.

14. Vibrational energy level transition requires a photon's wavelength shorter than 20 micrometer, usually in the infrared band. Vibration and rotation sometimes combine together to form vibration- rotation mode, the transition between vibration-rotation modes also involves certain frequencies.

15. c. Photodissociation Solar ultraviolet photon For photodissociation to occur, the wavelength of a photon must be in the ultraviolet band. To dissociate Oxygen the wavelength of radiation must be shorter than 200 nm. Ozone is a loosely bonded molecule. To dissociate a Ozone molecule, the frequency of a photon can be as low as 300 nm.

16. d. Electronic excitation 1st Shell2nd Shell e. Photoionization Electrons may be excited from one shell to another shell by a photon with a sufficiently high energy level. The wavelength is usually shorter than 1 micrometer. Photoelectron To photoionize a molecule requires the radiation with a wavelength shorter than 100 nm.

17. Electronic excitationPhotoionization M overlap Almost all solar radiations shorter than ultraviolet are used up in the upper layer for photoionization, electronic excitation, and molecule dissociation. Since most of solar energy is in the visible band, they have nothing to do with molecule vibration and rotation transition, so solar radiation can reach Earth's surface almost without any attenuation. On the other hand, terrestrial radiation in the infrared band, which is involved with atmospheric molecule vibration and rotation transitions, can be absorbed by the atmosphere to cause greenhouse effect.

18. Highly un-reactive greenhouse gases containing bonds of fluorine-carbon or fluorine-sulfur, such as Perfluorocarbons (CF4, C2F6, C3F8) and Sulfur Hexafluoride (SF6). These trace gases have strong absorption lines right in the atmospheric window.

19. Greenhouse effect: shortwave solar radiation is nearly transparent to the atmosphere, but longwave terrestrial radiation is trapped by greenhouse gases, causing the increase of surface temperature.

21. Radiative Equilibrium model

22. e=0 ----> radiative equilibrium model. e=1----> I=B In the real atmosphere, the absorbing materials are distributed continuously in the vertical. These include clouds, greenhouse gases such as water vapor, co2, O3,etc Too cold σ: emissivity

23. Effects of atmospheric convection If the Earth system were in a radiative equilibrium only, it would not be in a dynamic equilibrium because the air near surface will warm up by contacting with hot surface, thus, convection will happen. The situation is further complicated by the phase change of water. Difference between convection and advection

24. Heat Budget of Earth’s Atmosphere

26. Composition of the Atmosphere

27. Carbon Dioxide Water Vapor 0-4% by volumn Variable Components of the atmosphere

28. Aerosol - fine solid or liquid particles suspended in the air (0.001 to 10 )

29. Formation of Ozone Ozone Sustaining Ozone Depletion of Ozone 10-50 km (stratosphere)

30. Ozone Depletion Ozone

31. The Ozone Hole Ozone concentration drops sharply over Antarctica

32. The Ozone Hole Polar vortex Cold air -80C 1. Polar winter leading to the formation of circumpolar winds to develop the polar vortex which isolates the air within it. 2. Cold temperatures; cold enough for the formation of Polar Stratospheric Clouds. As the vortex air is isolated, the cold temperatures persist. 3. The chlorine reservoir species HCl and ClONO2 become very active on the surface of the polar stratospheric clouds. The most important reactions are:

33. Global Ozone Recovery Predictions Protecting the atmosphere’s ozone layer An international agreement known as the Montreal Protocol on substances that deplete the Ozone Layer was concluded under the auspices of United Nations in late 1987.

34. Temperature Thermal Structure of the Atmosphere Thermal Structure of the Atmosphere Temperature measures the average kinetic energy of molecules and atoms as they move.