Package blackbody

BlackBody simulates the color and the spectral distribution of a blackbody radiator at a given temperature.

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Description

Class Summary

BlackBody

Class BlackBody

Package blackbody Description

BlackBody simulates the color and the spectral distribution of a blackbody radiator at a given temperature.

The color of an object is depends upon its temperature as predicted by the Stefan-Boltzmann law. This law describes the radiation given off by an object above absolute zero. Every objects emits blackbody radiation although we do not normally notice it because our eyes are only sensitive to a very small portion of the electromagnetic spectrum. An object must be quite hot for it to emit visible light. For example, the heating element on a stove glows "red hot." The Stefan-Boltzmann law allows us to determine the temperature by measuring the radiation spectrum given off by this heating element. Our Sun is an another example of a blackbody radiator. It's spectrum isn't as smooth as the "ideal" ( it is pitted and bumpy due to real-world conditions including, but not limited to, absorption of the radiation en route to the earth) but it is close enough. It fact, measuring color is the primary means astronomers have of determining the temperatures of distant stars.

Documentation

• Embedding
• English resource file

Examples:

• Interactive mode
• Set Temperature

Additional BlackBody examples can be obtained from the Davidson College Physlets Site.