Lec13 - Assignments For Wed, Oct. 05 Do Online Exercise 08...

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Assignments For Wed, Oct. 05 Do Online Exercise 08 ("Doppler Effect" tutorial) For Mon, Oct. 10 Do Written HW#3
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Eqn summary: waves & light λ f = s • E = h f • F E = E/At = σ T 4 λ max =500 (T sun /T) Waves λ = wavelength f = frequency s= speed of wave (= c for light) Photon of light E = Energy h = Planck’s constant F E = radiative flux (energy E per area A and time t) T = temperature (in K) λ max = wavelength of maximum intensity (in nm)
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The Solar Spectrum
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Hydrogen energy levels
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Thermal Radiation
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1. Hotter objects emit more total Energy per unit surface area, or Energy F lux Stephan-Boltzmann Law F = σ T 4 2. Hotter objects emit bluer photons (with a higher average energy.) Wien Law λ max = 2.9 x 10 6 / T (K) [nm] Emission by Opaque Objects
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Luminosity & App. Brightness • Luminosity: L = σ T 4 4 π R 2 – or: L/L sun = (T/T sun ) 4 (R/R sun ) 2 • App. Brightness (aka 'Flux'): – B = F = L/4 π D 2
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Kirchhoff’s Laws 1 A hot, dense glowing object (solid or gas) emits a continuous spectrum.
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Kirchhoff’s Laws 2 A hot, low density gas emits light of only certain wavelengths -- an emission line spectrum.
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This note was uploaded on 02/01/2012 for the course PHYS 133 taught by Professor Staff during the Fall '08 term at University of Delaware.

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Lec13 - Assignments For Wed, Oct. 05 Do Online Exercise 08...

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