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Purpose: To apply radiation concepts learned in lecture to a mathematical and quantitative format. This will increase your understanding of radiation and further increase your confidence. Additionally, these concepts are important to understand Climate Change, and why our climate is warming with an increase in greenhouse gases, specifically CO2.
Learning Objectives: Calculate and evaluate the differences between the sun and earth's emitted radiation, and the impacts of the earth's atmosphere.
Stefan-Boltzmann Law: the total energy emitted by a body increases with temperature
E = σT4
where E is radiation emitted (units: W/m2), σ is the Stefan-Boltzmann constant (5.67x10-8 W/m2K4), and T is temperature (units: K).
Wien's Law: wavelength of radiative energy depends on temperature
where λ is the wavelength of emission (units: micrometers, microns, µm), C is Wien's constant (3000 µm*K), and T is temperature (units: K).
Part II: The Electromagnetic Spectrum
As defined in the previous part, wavelength is defined by an objects temperature. These wavelengths define how much energy is emitted and what electromagnetic wave it is emitted at (radio, microwave, infrared, etc.) .
Part III: The Earth's Energy Budget
Earths energy budgets incoming radiation is from the sun, but once it reaches Earth, there are many factors that lead to the reflection, absorption, and re-emission of said energy.
A handful of select gases in our atmosphere absorb certain wavelengths, which can lead to absorption and re-emission back towards Earth's surface.
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