8.5+Greenhouse+effect

IB Physics > Energy, Power and Climate Change =8.5 GREENHOUSE EFFECT= 8.5.1 Calculate the intensity of the Sun’s radiation incident on a planet. 8.5.2 Define //albedo//. 8.5.3 State factors that determine a planet’s albedo. Students should know that the Earth’s albedo varies daily and is dependent on season (cloud formations) and latitude. Oceans have a low value but snow a high value. The global annual mean albedo is 0.3 (30%) on Earth.
 * 8.1 Energy degradation and Power Generation || 8.2 World energy sources || 8.3 Fossil fuel power production || 8.4 Non-fossil fuel power production || 8.5 Greenhouse effect || 8.6 Global warming ||
 * Aim 7: ** Computer simulation, spreadsheets and databases have a significant role here.
 * Solar radiation **
 * The greenhouse effect **

[|HOW THE EFFECT WORKS -] Starts with a Bang blog

8.5.4 Describe the greenhouse effect.

[|GREENHOUSE EFFECT SIMULATION] - PhET

8.5.5 Identify the main greenhouse gases and their sources. The gases to be considered are CH 4, H 2 O, CO 2 and N 2 O. It is sufficient for students to know that each has natural and man-made origins. 8.5.6 Explain the molecular mechanisms by which greenhouse gases absorb infrared radiation. Students should be aware of the role played by resonance. The natural frequency of oscillation of the molecules of greenhouse gases is in the infrared region.

[|MOLECULES AND LIGHT SIMULATION] - PhET simulation

8.5.7 Analyse absorption graphs to compare the relative effects of different greenhouse gases. Students should be familiar with, but will not be expected to remember, specific details of graphs showing infrared transmittance through a gas. 8.5.8 Outline the nature of black-body radiation. Students should know that black-body radiation is the radiation emitted by a “perfect” emitter. media type="custom" key="11504998" 8.5.9 Draw and annotate a graph of the emission spectra of black bodies at different temperatures. 8.5.10 State the Stefan–Boltzmann law and apply it to compare emission rates from different surfaces. 8.5.11 Apply the concept of emissivity to compare the emission rates from the different surfaces. 8.5.12 Define //surface heat capacity C// s. Surface heat capacity is the energy required to raise the temperature of unit area of a planet’s surface by one degree, and is measured in J m -2 K -1 8.5.13 Solve problems on the greenhouse effect and the heating of planets using a simple energy balance climate model. Students should appreciate that the change of a planet’s temperature over a period of time is given by: (incoming radiation intensity – outgoing radiation intensity)*time / surface heat capacity. Students should be aware of limitations of the model and suggest how it may be improved.