Blackbody Spectrum

Requires a Wolfram Notebook System

Interact on desktop, mobile and cloud with the free Wolfram Player or other Wolfram Language products.

Planck's law gives the intensity of the energy radiated by a blackbody as a function of wavelength and temperature. As the temperature of a blackbody increases, the peak wavelength shifts from red to blue. Extremely hot blackbodies emit most of their energy in the ultraviolet range, while cool blackbodies emit primarily in the infrared. Stars behave like blackbodies, so their color follows their temperature, too. Stars similar to the sun (with a temperature of about 5800 Kelvin) appear nearly white because the visible part of the intensity curve is nearly flat.

Contributed by: Jeff Bryant (April 2007)
Open content licensed under CC BY-NC-SA


Snapshots


Details

Snapshot 1: Cool stars are orange or red.

Snapshot 2: Medium temperature stars are nearly white.

Snapshot 3: Hot stars are blue.



Feedback (field required)
Email (field required) Name
Occupation Organization
Note: Your message & contact information may be shared with the author of any specific Demonstration for which you give feedback.
Send