Syllabus & Lecture Notes
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1 I. SYLLABUS AND INTRODUCTION Let us start with a brief overview of the items that will (hopefully) be covered in this course and to give a guideline of what we are trying to learn. Quantum mechanics 660 and 661 are advanced quantum mechanics courses designed for graduate students. The courses will be treated as a one-year course. It will be assumed that students have already some background in quantum mechanics (the concepts of waves, quantization, expectation values, etc.). An advised introductory text- book is Introduction to quantum mechanics by Griffiths. A number of things will, however, be repeated albeit in a more mathematical fashion. Also some basic knowledge in Fourier analysis, differential equations and linear algebra (calculation of eigenvalues and eigenstates) will be expected. All the information you need to know are in the lecture notes. However, the lecture notes are relatively concise and further reading is recommended. The book that was used last year was Liboff, Introductory Quantum Mechanics, fourth edition. However, a lot of other books treat the material of 660 in a similar fashion, so pick a book that you like best. Some of the material is not covered in Liboff (the older editions don’t have relativistic quantum mechanics and quite a bit of the material of 661 is not in there). The course is developed from a physicists point of view. Some concepts and mathematical techniques will be intro- duced along the way (such as matrix techniques) under the assumption that most of you are already somewhat familiar with them (after all, there are also 3 and 4 hundred level quantum mechanics courses). For a more comprehensive view of those things, I will refer to the textbook. The subjects that will be covered are History, Planck’s quantum hypothesis, photoelectric effect,specific heat, atomic physics. • The introduction is somewhat different from what is usually given in textbooks. However, since most of you have already followed a quantum mechanics course and since this is a graduate course, I think it is interesting to do it this way. Quite some time will be devoted to Planck’s hypothesis. The physical language is quite different from that of the rest of the course (it is more thermodynamics than quantum mechanics). Some of these things are treated in the exercizes of Chapter 2 of Liboff. Other things will be mentioned more briefly. Wave mechanics, Schr¨odinger equation, probability density, free particles, Heisenberg’s uncertainty principle. • This section tries to show some of the thinking that led to the Schr¨odinger equation. As soon as you leave the idea of a particle as a billiard ball behind you, a number of other things follow directly, such as Heisenberg’s uncertainty principle. Harmonic oscillator, Schr¨odinger equation approach, Solution using operators, Operators and wavefunctions, • Correspondence principle. Although most of you have seen the harmonic oscillator already, it is an important example, since the number of exactly solvable models in quantum mechanics is limited. Try to pay special attention to the two approaches to attack this problem. The Schr¨odinger approach, solving the differential equation for the wavefunction, and the algebraic or operator approach due to Heisenberg, Jordan, and Born. Although the Schr¨odinger approach is more intuitive, the operator approach will become more important as we go on, since often we do not really care that much about the wavefunction, but we are more interested in the spectral properties (energies) Of the problem. The Hydrogen atom, Legendre polynomials, angular momentum, matrix notation. • Again pay attention to the dual approach to this problem. The Schr¨odinger approach (solving the wavefunction) and the operator approach (angular momentum). This involves quite a bit of mathematics (solving differential equations). Here we will only deal with the potential from the nucleus, leading to the orbitals of the atom. Other aspects follow in the next section. Relativistic quantum mechanics, Klein-Gordan equation, Dirac equation, spin-orbit coupling. • This section introduces the Dirac equation and its consequences for the problems that we are interested in: the introduction of spin, relativistic correction to the Hydrogen atom (spin-orbit coupling, lowest order kinetic corrections). We could introduce (which would have been simpler) these aspects in a phenomenological or semi quantum/classical approach, but this is more fun and avoids having to treat relativistic quantum mechanics as some appendix. Note that we are not really interested in things such as time dilation, length contraction, etc. Perturbation theory and absorption and emission of photons, time-independent perturbation theory, • time-dependent perturbation theory, interaction of radiation and atom To be able to describe the emission and absortion of photons by an atom, we discuss perturbation theory. This will be done in some detail because of its relevance to later problems. Many-electron atom Pauli’s exclusion principle, the Helium atom, periodic table, Coulomb interactions, • addition of angular momenta. 2 FIG. 1: Left: The radiation spectrum of the sun at the top of the atmosphere (yellow) and at sea level (red) compared with a blackbody spectrum for 5250◦C. Right: Max Planck in 1901, around the time he developed the law now named after him. Source: wikipedia Having solved the atom for one electron, we would like to fill it with more electrons. First, we need to discuss a peculiar aspect of electrons (or fermions in general), namely the exclusion principle. We start with the simplest many-electron atom, Helium. We soon discover that electron-electron interaction have a strong influence and see that things are not as simple as suggested by the Hydrogen atom solution. We continue with a more general discussion of Coulomb interaction between electrons and how to couple the electron wavefunction in a smart way (LS-coupling). Molecules and solids, Hydrogen molecule, solids, (nearly) free-electron model. • We then continue by taking two atoms amd bringing them close together, thereby forming a molecule. If we continue adding atoms, we can form a one-dimensional solid, this is known as a tight-binding approximation. We can also approach it from the other side, by viewing a solid as a box of free electrons. The periodic potential has a only a small, but important, effect. Second quantization, the Coulomb gas. • We have a look at the ground-state energy of the electron gas and calculate it in the Hartree-Fock limit. We also see what the effect are of screening. II. OLD QUANTUM MECHANICS A. Planck’s quantum hypothesis The quantum theory started with the blackbody radiation. All matter emits electromagnetic radiation when its temperature is above abolute zero. The radiation results from the conversion of thermal energy into electromagnetic energy. A black body is a systems that absorbs all incident radiation. On the other hand, this also makes it the best possible emitter. It is hard to find a perfect black body, but, for example, graphite, is a good approximation. However, even when a system is not a perfect black body, the basic phenomena remains the same. The sun can, for example, be described to a good approximation as a black body, see Fig. 1. The spectral distribution has a maximum and decays for small and large wavelengths. For the sun which has an effective temperature of around 5500 K, the maximum lies in the visible region of the electromagnetic spectrum and is inherently related to the fact that the sun is white (and not yellow or even yellowish). Before Max Planck took up the subject there was already a surprising 3 Intensity Harb. un.L 0.25 0.20 0.15 0.10 0.05 E HeVL 0 1 2 3 4 5 FIG. 2: The blue line shows the Planck distribution as a function of energy for T = 5523 K. The brown line shows Wien’s distribution curve. The magenta line is the Rayleigh-Jeans law. amount of understanding of the spectral distribution predominantly due to Wilhelm Wien (1864-1928). For his work, he received the Nobel prize for Physics in 1911. Using general thermodynamic arguments, Wien showed in 1893 that the energy dependence is given by ω u(ω)= ω3f( ), (1) T where ω = 2πν and f is a function that only depends on the ratio ω/T , where T is the temperature. The function ω f( T ) cannot be derived from these considerations, but it can only be a function of ω/T or λT when expressed in the wavelength λ. The consequence of that is that the maximum occurs at a particular value of T/λ. Therefore, if the temperature changes the maximum occurs at a different wavelength. The human body can also be viewed as a far-from-perfect black body. The maximum occurs for a wavelength 9 λmax,SunTSun 525 10− 5500 λmax,human = = × = 9 µm, (2) Thuman 310 ∼ ω which is in the far infrared. Obviously, we would like to understand that the function f( T ) is. Wien made an ω educated guess that f( T ) = exp( aω/T ), where a is a constant. This dependence was obviously inspired by the Boltzmann factor and is a surprisingly− good guess, see Fig. 2. However, there is something strange about using the Boltzmann factor. The factor exp( E/kBT ), where kB is Boltzmann’s constant, implies that there is some finite energy associated with exciting electromagnetic− radiation. This is in complete contradiction with the classical way of thinking. The energy density of electro-magnetic radiation is given by 1 ε E2 + 1 B2, and therefore determined by 2 0 2µ0 the magnitudes of the electric and magnetic fields. Since we can take any possible value of these fields, any possible value of of the energy density is possible.