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Quantum physics quantum theory, quantum mechanics PowerPoint Presentation
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Quantum physics quantum theory, quantum mechanics

Quantum physics quantum theory, quantum mechanics

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Quantum physics quantum theory, quantum mechanics

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    1. Quantum physics (quantum theory, quantum mechanics) Part 1:

    2. Outline Introduction Problems of classical physics emission and absorption spectra Black-body Radiation experimental observations Wiens displacement law Stefan Boltzmann law Rayleigh - Jeans Wiens radiation law Plancks radiation law photoelectric effect observation studies Einsteins explanation Summary

    3. Question: What do these have in common? lasers solar cells transistors computer chips CCDs in digital cameras superconductors ......... Answer: They are all based on the quantum physics discovered in the 20th century.

    4. Why Quantum Physics? Classical Physics: developed in 15th to 20th century; provides very successful description of every day, ordinary objects motion of trains, cars, bullets,. orbit of moon, planets how an engine works,.. subfields: mechanics, thermodynamics, electrodynamics, Quantum Physics: developed early 20th century, in response to shortcomings of classical physics in describing certain phenomena (blackbody radiation, photoelectric effect, emission and absorption spectra) describes small objects (e.g. atoms and their constituents)

    5. Quantum Physics QP is weird and counterintuitive Those who are not shocked when they first come across quantum theory cannot possibly have understood it (Niels Bohr) Nobody feels perfectly comfortable with it (Murray Gell-Mann) I can safely say that nobody understands quantum mechanics (Richard Feynman) But: QM is the most successful theory ever developed by humanity underlies our understanding of atoms, molecules, condensed matter, nuclei, elementary particles Crucial ingredient in understanding of stars,

    6. Features of QP Quantum physics is basically the recognition that there is less difference between waves and particles than was thought before key insights: light can behave like a particle particles (e.g. electrons) are indistinguishable particles can behave like waves (or wave packets) waves gain or lose energy only in "quantized amounts detection (measurement) of a particle ? wave will change suddenly into a new wave quantum mechanical interference amplitudes add QP is intrinsically probabilistic what you can measure is what you can know

    7. emission spectra continuous spectrum solid, liquid, or dense gas emits continuous spectrum of electromagnetic radiation (thermal radiation); total intensity and frequency dependence of intensity change with temperature (Kirchhoff, Bunsen, Wien, Stefan, Boltzmann, Planck) line spectrum rarefied gas which is excited by heating, or by passing discharge through it, emits radiation consisting of discrete wavelengths (line spectrum) wavelengths of spectral lines are characteristic of atoms

    9. Emission spectra:

    10. Absorption spectra first seen by Fraunhofer in light from Sun; spectra of light from stars are absorption spectra (light emitted by hotter parts of star further inside passes through colder atmosphere of star) dark lines in absorption spectra match bright lines in discrete emission spectra see dark lines in continuous spectrum Helium discovered by studying Sun's spectrum light from continuous-spectrum source passes through colder rarefied gas before reaching observer;

    11. Fraunhofer spectra

    12. Spectroscopic studies

    13. Thermal radiation thermal radiation = e.m. radiation emitted by a body by virtue of its temperature spectrum is continuous, comprising all wavelengths thermal radiation formed inside body by random thermal motions of its atoms and molecules, repeatedly absorbed and re-emitted on its way to surface ? original character of radiation obliterated ? spectrum of radiation depends only on temperature, not on identity of object amount of radiation actually emitted or absorbed depends on nature of surface good absorbers are also good emitters (why??)

    14. warm bodies emit radiation

    15. Black-body radiation Black body perfect absorber ideal body which absorbs all e.m. radiation that strikes it, any wavelength, any intensity such a body would appear black ? black body must also be perfect emitter able to emit radiation of any wavelength at any intensity -- black-body radiation Hollow cavity (Hohlraum) kept at constant T hollow cavity with small hole in wall is good approximation to black body thermal equilibrium inside, radiation can escape through hole, looks like black-body radiation

    16. Studies of radiation from hollow cavity behavior of radiation within a heated cavity studied by many physicists, both theoretically and experimentally Experimental findings: spectral density ?(n,T) (= energy per unit volume per unit frequency) of the heated cavity depends on the frequency n of the emitted light and the temperature T of the cavity and nothing else.

    17. Black-body radiation spectrum Measurements of Lummer and Pringsheim (1900) calculation

    18. various attempts at descriptions: peak vs temperature: ?max T = C (Wiens displacement law), C= 2.898 10-3 m K total emitted power (per unit emitting area) P = sT4 (Stefan-Boltzmann), s = 5.672 10-8 W m-2 K-4 Wilhelm Wien (1896) r(n,T) = a n3 e-bn /T, (a and b constants). OK for high frequency but fails for low frequencies. Rayleigh-Jeans Law (1900) r(n,T) = a n2 T (a = constant). (constant found to be = 8pk/c3 by James Jeans, in 1906) OK for low frequencies, but ultra violet catastrophe at high frequencies

    19. Ultraviolet catastrophe

    21. Plancks quantum hypothesis Max Planck (Oct 1900) found formula that reproduced the experimental results derivation from classical thermodynamics, but required assumption that oscillator energies can only take specific values E = 0, h?, 2h?, 3h?, (using Boltzmann factor W(E) = e-E/kT )

    22. Consequences of Plancks hypothesis oscillator energies E = nh?, n = 0,1,; h = 6.626 10-34 Js = 4.13 10-15 eVs now called Plancks constant ? oscillators energy can only change by discrete amounts, absorb or emit energy in small packets quanta; Equantum = h? average energy of oscillator <Eosc> = h?/(ex 1) with x = h?/kT; for low frequencies get classical result <Eosc> = kT, k = 1.38 10-23 JK-1

    23. Frequencies in cavity radiation cavity radiation = system of standing waves produced by interference of e.m. waves reflected between cavity walls many more modes per wavelength band ?? at high frequencies (short wavelengths) than at low frequencies for cavity of volume V, ?n = (8pV/?4) ?? or ?n = (8pV/c3) ?2 ? ? if energy continuous, get equipartition, <E> = kT ? all modes have same energy ? spectral density grows beyond bounds as ??? If energy related to frequency and not continous (E = nh?), the Boltzmann factor e-E/kT leads to a suppression of high frequencies

    24. Problems estimate Suns temperature assume Earth and Sun are black bodies Stefan-Boltzmann law Earth in thermal equilibrium (i.e. rad. power absorbed = rad. power emitted) , mean temperature T = 290K Suns angular size ?Sun = 32 show that for small frequencies, Plancks average oscillator energy yields classical equipartition result <Eosc> = kT show that for standing waves on a string, number of waves in band between ? and ?+?? is ?n = (2L/?2) ??

    25. Summary classical physics explanation of black-body radiation failed Plancks ad-hoc assumption of energy quanta of energy Equantum = h?, modifying Wiens radiation law, leads to a radiation spectrum which agrees with experiment. old generally accepted principle of natura non facit saltus violated Opens path to further developments