Download
general physics phy 2140 n.
Skip this Video
Loading SlideShow in 5 Seconds..
General Physics (PHY 2140) PowerPoint Presentation
Download Presentation
General Physics (PHY 2140)

General Physics (PHY 2140)

344 Vues Download Presentation
Télécharger la présentation

General Physics (PHY 2140)

- - - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript

  1. General Physics (PHY 2140) Lecture 16 • Modern Physics • Atomic Physics • Early models of the atom • Atomic spectra • Bohr’s theory of hydrogen • De Broglie wavelength in the atom • Quantum mechanics and Spin Chapter 28 http://www.physics.wayne.edu/~alan/2140Website/Main.htm

  2. Lightning Review • Last lecture: • Quantum physics • Wave function • Uncertainty relations Review Problem: If matter has a wave structure, why is this not observable in our daily experiences? (baseball)  10-34 m

  3. 27.9 The Uncertainty Principle • When measurements are made, the experimenter is always faced with experimental uncertainties in the measurements • Classical mechanics offers no fundamental barrier to ultimate refinements in measurements • Classical mechanics would allow for measurements with arbitrarily small uncertainties

  4. The Uncertainty Principle • Quantum mechanics predicts that a barrier to measurements with ultimately small uncertainties does exist • In 1927 Heisenberg introduced the uncertainty principle • If a measurement of position of a particle is made with precision Δx and a simultaneous measurement of linear momentum is made with precision Δp, then the product of the two uncertainties can never be smaller than h/4

  5. The Uncertainty Principle • Mathematically, • It is physically impossible to measure simultaneously the exact position and the exact linear momentum of a particle • Another form of the principle deals with energy and time:

  6. Thought Experiment – the Uncertainty Principle • A thought experiment for viewing an electron with a powerful microscope • In order to see the electron, at least one photon must bounce off it • During this interaction, momentum is transferred from the photon to the electron • Therefore, the light that allows you to accurately locate the electron changes the momentum of the electron

  7. Problem: macroscopic uncertainty A 50.0-g ball moves at 30.0 m/s. If its speed is measured to an accuracy of 0.10%, what is the minimum uncertainty in its position?

  8. A 50.0-g ball moves at 30.0 m/s. If its speed is measured to an accuracy of 0.10%, what is the minimum uncertainty in its position? Notice that the ball is non-relativistic. Thus, p = mv, and uncertainty in measuring momentum is Given: v = 30 m/s Dv/v = 0.10% m = 50.0 g Find: dx = ? Thus, uncertainty relation implies Too small to measure!!

  9. Problem: Macroscopic measurement A 0.50-kg block rests on the icy surface of a frozen pond, which we can assume to be frictionless. If the location of the block is measured to a precision of 0.50 cm, what speed must the block acquire because of the measurement process? Recall: and

  10. Atomic physics: Chapter 28

  11. Importance of Hydrogen Atom • Hydrogen is the simplest atom • The quantum numbers used to characterize the allowed states of hydrogen can also be used to describe (approximately) the allowed states of more complex atoms • This enables us to understand the periodic table • The hydrogen atom is an ideal system for performing precise comparisons of theory and experiment • Also for improving our understanding of atomic structure • Much of what we know about the hydrogen atom can be extended to other single-electron ions • For example, He+ and Li2+

  12. Early Models of the Atom • J.J. Thomson’s model of the atom • A volume of positive charge • Electrons embedded throughout the volume • A change from Newton’s model of the atom as a tiny, hard, indestructible sphere “watermelon” model

  13. Experimental tests • Expect: • Mostly small angle scattering • No backward scattering events • Results: • Mostly small scattering events • Several backward scatterings!!!

  14. Early Models of the Atom • Rutherford’s model • Planetary model • Based on results of thin foil experiments • Positive charge is concentrated in the center of the atom, called the nucleus • Electrons orbit the nucleus like planets orbit the sun

  15. Problem: Rutherford’s model The “size” of the atom in Rutherford’s model is about 1.0 × 10–10 m. (a) Determine the attractive electrical force between an electron and a proton separated by this distance. (b) Determine (in eV) the electrical potential energy of the atom.

  16. The “size” of the atom in Rutherford’s model is about 1.0 × 10–10 m. (a) Determine the attractive electrical force between an electron and a proton separated by this distance. (b) Determine (in eV) the electrical potential energy of the atom. Electron and proton interact via the Coulomb force Given: r = 1.0 × 10–10 m Find: F = ? PE = ? Potential energy is

  17. Difficulties with the Rutherford Model • Atoms emit certain discrete characteristic frequencies of electromagnetic radiation • The Rutherford model is unable to explain this phenomena • Rutherford’s electrons are undergoing a centripetal acceleration and so should radiate electromagnetic waves of the same frequency, thus leading to electron “falling on a nucleus” in about 10-12 seconds!!! • The radius should steadily decrease as this radiation is given off • The electron should eventually spiral into the nucleus • It doesn’t

  18. 28.2 Emission Spectra • A gas at low pressure has a voltage applied to it • A gas emits light characteristic of the gas • When the emitted light is analyzed with a spectrometer, a series of discrete bright lines is observed • Each line has a different wavelength and color • This series of lines is called an emission spectrum

  19. Emission Spectrum of Hydrogen • The wavelengths of hydrogen’s spectral lines can be found from • RH is the Rydberg constant • RH = 1.0973732 x 107 m-1 • n is an integer, n = 1, 2, 3, … • The spectral lines correspond to different values of n • A.k.a. Balmer series • Examples of spectral lines • n = 3, λ = 656.3 nm • n = 4, λ = 486.1 nm

  20. Absorption Spectra • An element can also absorb light at specific wavelengths • An absorption spectrum can be obtained by passing a continuous radiation spectrum through a vapor of the gas • The absorption spectrum consists of a series of dark lines superimposed on the otherwise continuous spectrum • The dark lines of the absorption spectrum coincide with the bright lines of the emission spectrum

  21. Applications of Absorption Spectrum • The continuous spectrum emitted by the Sun passes through the cooler gases of the Sun’s atmosphere • The various absorption lines can be used to identify elements in the solar atmosphere • Led to the discovery of helium (from helios)

  22. 28.3 The Bohr Theory of Hydrogen • In 1913 Bohr provided an explanation of atomic spectra that includes some features of the currently accepted theory • His model includes both classical and non-classical ideas • His model included an attempt to explain why the atom was stable

  23. Bohr’s Assumptions for Hydrogen • The electron moves in circular orbits around the proton under the influence of the Coulomb force of attraction • The Coulomb force produces the centripetal acceleration • Only certain electron orbits are stable • These are the orbits in which the atom does not emit energy in the form of electromagnetic radiation • Therefore, the energy of the atom remains constant and classical mechanics can be used to describe the electron’s motion • Radiation is emitted by the atom when the electron “jumps” from a more energetic initial state to a lower state • The “jump” cannot be treated classically

  24. Bohr’s Assumptions • More on the electron’s “jump”: • The frequency emitted in the “jump” is related to the change in the atom’s energy • It is generally not the same as the frequency of the electron’s orbital motion • The size of the allowed electron orbits is determined by a condition imposed on the electron’s orbital angular momentum

  25. Results • The total energy of the atom • Newton’s law • This can be used to rewrite kinetic energy as • Thus, the energy can also be expressed as

  26. Bohr Radius • The radii of the Bohr orbits are quantized ( ) (from quantized angular momentum: mevr = nħ and Newtons law) • This shows that the electron can only exist in certain allowed orbits determined by the integer n • When n = 1, the orbit has the smallest radius, called the Bohr radius, ao • ao = 0.0529 nm

  27. Radii and Energy of Orbits • A general expression for the radius of any orbit in a hydrogen atom is • rn = n2 ao • The energy of any orbit is • En = - 13.6 eV/ n2 • The lowest energy state is called the ground state • This corresponds to n = 1 • Energy is –13.6 eV • The next energy level has an energy of –3.40 eV • The energies can be compiled in an energy level diagram • The ionization energy is the energy needed to completely remove the electron from the atom (n = ∞, E = 0) • The ionization energy for hydrogen is 13.6 eV

  28. Energy Level Diagram • The value of RH from Bohr’s analysis is in excellent agreement with the experimental value • A more generalized equation can be used to find the wavelengths of any spectral lines • For the Balmer series, nf = 2 • For the Lyman series, nf = 1 • Whenever a transition occurs between a state, ni and another state, nf (where ni > nf), a photon is emitted • The photon has a frequency f = (Ei – Ef)/h and wavelength λ

  29. Problem: Transitions in the Bohr’s model A photon is emitted as a hydrogen atom undergoes a transition from the n = 6 state to the n = 2 state. Calculate the energy and the wavelength of the emitted photon.

  30. A photon is emitted as a hydrogen atom undergoes a transition from the n = 6 state to the n = 2 state. Calculate the energy and the wavelength of the emitted photon. From or With ni = 6 and nf = 2 we have: Given: ni = 6 nf = 2 Find: l = ? Eg= ? The Photon energy is:

  31. Bohr’s Correspondence Principle • Bohr’s Correspondence Principle states that quantum mechanics is in agreement with classical physics when the energy differences between quantized levels are very small • Similar to having Newtonian Mechanics be a special case of relativistic mechanics when v << c

  32. Successes of the Bohr Theory • Explained several features of the hydrogen spectrum • Accounts for Balmer and other series • Predicts a value for RH that agrees with the experimental value • Gives an expression for the radius of the atom • Predicts energy levels of hydrogen • Gives a model of what the atom looks like and how it behaves • Can be extended to “hydrogen-like” atoms • Those with one electron • Ze2 needs to be substituted for e2 in equations • Z is the atomic number of the element

  33. Recall Bohr’s Assumptions • Only certain electron orbits are stable. Radiation is emitted by the atom when the electron “jumps” from a more energetic initial state to a lower state • The size of the allowed electron orbits is determined by a condition imposed on the electron’s orbital angular momentum Why is that?

  34. Modifications of the Bohr Theory – Elliptical Orbits • Sommerfeld extended the results to include elliptical orbits • Retained the principle quantum number, n • Added the orbital quantum number, ℓ • ℓ ranges from 0 to n-1 in integer steps • All states with the same principle quantum number are said to form a shell • The states with given values of n and ℓ are said to form a subshell

  35. Modifications of the Bohr Theory – Zeeman Effect and fine structure • Another modification was needed to account for the Zeeman effect • The Zeeman effect is the splitting of spectral lines in a strong magnetic field • This indicates that the energy of an electron is slightly modified when the atom is immersed in a magnetic field • A new quantum number, mℓ, called the orbital magnetic quantum number, had to be introduced • m ℓ can vary from - ℓ to + ℓ in integer steps • High resolution spectrometers show that spectral lines are, in fact, two very closely spaced lines, even in the absence of a magnetic field • This splitting is called fine structure • Another quantum number, ms, called the spin magnetic quantum number, was introduced to explain the fine structure

  36. 28.5 de Broglie Waves • One of Bohr’s postulates was the angular momentum of the electron is quantized, but there was no explanation why the restriction occurred • de Broglie assumed that the electron orbit would be stable only if it contained an integral number of electron wavelengths

  37. de Broglie Waves in the Hydrogen Atom • In this example, three complete wavelengths are contained in the circumference of the orbit • In general, the circumference must equal some integer number of wavelengths but , so This was the first convincing argument that the wave nature of matter was at the heart of the behavior of atomic systems

  38. In an analysis relating Bohr's theory to the de Broglie wavelength of electrons, when an electron moves from the n = 1 level to the n = 3 level, the circumference of its orbit becomes 9 times greater. This occurs because (a) there are 3 times as many wavelengths in the new orbit, (b) there are 3 times as many wavelengths and each wavelength is 3 times as long, (c) the wavelength of the electron becomes 9 times as long, or (d) the electron is moving 9 times as fast. QUICK QUIZ 1 (b). The circumference of the orbit is n times the de Broglie wavelength (2πr = nλ), so there are three times as many wavelengths in the n = 3 level as in the n = 1 level.

  39. 28.6 Quantum Mechanics and the Hydrogen Atom • One of the first great achievements of quantum mechanics was the solution of the wave equation for the hydrogen atom • The significance of quantum mechanics is that the quantum numbers and the restrictions placed on their values arise directly from the mathematics and not from any assumptions made to make the theory agree with experiments

  40. Problem: wavelength of the electron Determine the wavelength of an electron in the third excited orbit of the hydrogen atom, with n = 4.

  41. Determine the wavelength of an electron in the third excited orbit of the hydrogen atom, with n = 4. Recall that de Broglie’s wavelength of electron depends on its momentum, l = h/(mev). Let us find it, Given: n = 4 Find: le = ? Recall that Thus,

  42. Quantum Number Summary • The values of n can increase from 1 in integer steps • The values of ℓ can range from 0 to n-1 in integer steps • The values of mℓ can range from -ℓ to ℓ in integer steps

  43. How many possible orbital states are there for (a) the n = 3 level of hydrogen? (b) the n = 4 level? QUICK QUIZ 2 The quantum numbers associated with orbital states are n, , and m. For a specified value of n, the allowed values of  range from 0 to n – 1. For each value of , there are (2  + 1) possible values of m. (a) If n = 3, then  = 0, 1, or 2. The number of possible orbital states is then [2(0) + 1] + [2(1) + 1] + [2(2) + 1] = 1 + 3 + 5 = 9. (b) If n = 4, one additional value of  is allowed ( = 3) so the number of possible orbital states is now 9 + [2(3) + 1] = 9 + 7 = 16 (each is n2)

  44. Spin Magnetic Quantum Number • It is convenient to think of the electron as spinning on its axis • The electron is not physically spinning • There are two directions for the spin • Spin up, ms = ½ • Spin down, ms = -½ • There is a slight energy difference between the two spins and this accounts for the Zeeman effect • Sodium D lines are an example of this splitting.

  45. Electron Clouds • The graph shows the solution to the wave equation for hydrogen in the ground state • The curve peaks at the Bohr radius • The electron is not confined to a particular orbital distance from the nucleus • The probability of finding the electron at the Bohr radius is a maximum

  46. Electron Clouds • The wave function for hydrogen in the ground state is symmetric • The electron can be found in a spherical region surrounding the nucleus • The result is interpreted by viewing the electron as a cloud surrounding the nucleus • The densest regions of the cloud represent the highest probability for finding the electron