In the graph above are shown 2 blackbody curves, with log Flux plotted against log
.
The yellow curve shows the flux emitted by a 5000° K blackbody,
the approximate temperature of our star, the Sun. You may change the
temperature of the second blackbody curve shown by entering a new value
in the text entry box below the graph. The total range available
is from 2000° K to 30000 ° K.
Note that the emission of the hotter object is larger at all wavelengths than that of a cooler object. The emission of hotter objects extends much farther to the blue (short wavelengths) but relatively less toward the red than does the flux of cooler objects. The wavelength of the peak of the emission curve moves toward the blue as objects get hotter.
Wien Distribution
Rayleigh-Jeans Distribution
Wien Displacement Law
Stefan-Boltzmann Law
Constants
This VRML + HTML package on Blackbody emission was constructed by Karen M. Strom. Contact your local instructor for help if it is used as part of your class.