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S10P1CLec27A - Physics 1C Lecture 27A"Any other situation...

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Physics 1C Lecture 27A "Any other situation in quantum mechanics, it turns out, can always be explained by saying, ‘You remember the experiment with the two holes? It’s the same thing.’ " --Richard Feynman
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Blackbody Radiation An object at any temperature emits electromagnetic radiation (also called thermal radiation). Stefan’s Law describes the total power radiated. The spectrum of radiation depends on the temperature and properties of the object. As the temperature increases, the peak of the intensity shifts to shorter wavelengths.
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Blackbody Radiation A blackbody is any body that is a perfect absorber or emitter of light. The wavelength of the peak of the blackbody distribution was found to follow Wien’s Displacement Law: λ max T = 0.2898 x 10 -2 m • K where λ max is the wavelength at which the curve’s peak. T is the absolute temperature of the object emitting the radiation.
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Blackbody Radiation The experimental data of the emitted blackbody radiation did not match with what classical theory predicted. Classical theory predicted infinite energy at very short wavelengths, but experiment displayed no energy at short wavelengths. This contradiction is called the ultraviolet catastrophe.
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Planck’s Solution Max Planck hypothesized that blackbody radiation was produced by submicroscopic charge oscillators known as resonators.
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