Chapter 34: Problem 39
Treating the Sun as a \(5800-\mathrm{K}\) blackbody, compare its UV radiance at 200 nm with its visible radiance at its 500 -nm peak wavelength.
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Chapter 34: Problem 39
Treating the Sun as a \(5800-\mathrm{K}\) blackbody, compare its UV radiance at 200 nm with its visible radiance at its 500 -nm peak wavelength.
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Show that in the Bohr model, the frequency of a photon emitted in a transition between levels \(n+1\) and \(n,\) in the limit of large \(n\) is equal to the electron's orbital frequency. (This is an example of Bohr's correspondence principle.)
The maximum electron energy in a photoelectric experiment is \(2.8 \mathrm{eV} .\) When the wavelength of the illuminating radiation is increased by \(50 \%,\) the maximum energy drops to \(1.1 \mathrm{eV}\). Find (a) the work function of the emitting surface and (b) the original wavelength.
The converse approach is used for particles with longer lifetimes: Direct measurement of the lifetime yields, through energy-time uncertainty, a range of expected values for particle energies or masses. The longer the lifetime, a. the wider the mass range and the narrower the energy range. b. the wider the mass and energy ranges. c. the narrower the mass range and the wider the energy range. d. the narrower the mass and energy ranges.
Imagine an atom that, unlike hydrogen, had only three energy levels. If these levels were evenly spaced, how many spectral lines would result? How would their wavelengths compare?
How slowly must an electron be moving for its de Broglie wavelength to be \(1 \mathrm{mm} ?\)
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