Stefan Boltzmann Law and Emissivity

The Stefan Boltzmann law of radiation is an equation to determine the emissive power, which is just the rate of energy emitted by a blackbody per unit area of surface. Through multiplying by the area the Stefan Boltzmann law can also tell you how much energy a given surface is emitting per time. Lastly, for grey surfaces (surfaces that are not blackbodies), a correcting term (an object's emissivity) is added.

This timeline is meant to help you better understand the Stefan-Boltzmann law and emissivity:
0:00 Introduction.
0:06 The Stefan Boltzmann Law Definition
0:12 Review of BlackBody Radiation
0:28 What is an ideal body?
0:41 Stefan Boltzmann Law Equation
1:47 Emissivity
2:45 Outro

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This video is part of our Heat Transfer course. Heat Transfer is an interesting field of study and focuses primarily around the three modes of heat transfer, that is conduction, convection and radiation. This is taught in just about all engineering courses and I hope that this playlist will make what is typically considered a tough course much easier for you.
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