The calculation of the Hamiltonian proceeds as before, all the way through to thepenultimate line (5.11). At that stage, we get∫d 3 p[ ]H =(2π) E 3 ⃗p b s †⃗p bs ⃗p − cs ⃗p cs †⃗p∫d 3 p[]=(2π) E 3 ⃗p b s †⃗p bs ⃗p + cs †⃗p cs ⃗p − (2π)3 δ (3) (0)(5.17)The anti-commutators have saved us from the indignity of an unbounded Hamiltonian.Note that when normal ordering the Hamiltonian we now throw away a negative contribution−(2π) 3 δ (3) (0). In principle, this could partially cancel the positive contributionfrom bosonic fields. Cosmological constant problem anyone?!5.2.1 Fermi-Dirac StatisticsJust as in the bosonic case, we define the vacuum |0〉 to satisfy,b s ⃗p |0〉 = cs ⃗p |0〉 = 0 (5.18)Although b and c obey anti-commutation relations, the Hamiltonian (5.17) has nicecommutation relations with them. You can check that[H, b r ⃗p ] = −E ⃗p b r ⃗p and [H, b r †⃗p ] = E ⃗p b r †⃗p[H, c r ⃗p] = −E ⃗p c r ⃗p and [H, c r †⃗p ] = E ⃗p c r †⃗p(5.19)This means that we can again construct a tower of energy eigenstates by acting on thevacuum by b r †⃗pand c r,†⃗pto create particles and antiparticles, just as in the bosonic case.For example, we have the one-particle statesThe two particle states now satisfy|⃗p, r〉 = b r †⃗p|0〉 (5.20)|⃗p 1 , r 1 ; ⃗p 2 , r 2 〉 ≡ b r 1 †⃗p 1b r 2 †⃗p 2|0〉 = − |⃗p 2 , r 2 ; ⃗p 1 , r 1 〉 (5.21)confirming that the particles do indeed obey Fermi-Dirac statistics. In particular, wehave the Pauli-Exclusion principle |⃗p, r;⃗p, r〉 = 0. Finally, if we wanted to be sureabout the spin of the particle, we could act with the angular momentum operator(4.96) to confirm that a stationary particle |⃗p = 0, r〉 does indeed carry intrinsic angularmomentum 1/2 as expected.5.3 Dirac’s Hole Interpretation“In this attempt, the success seems to have been on the side of Dirac ratherthan logic”Pauli on Dirac– 110 –
Let’s pause our discussion to make a small historical detour. Dirac originally viewedhis equation as a relativistic version of the Schrödinger equation, with ψ interpretedas the wavefunction for a single particle with spin. To reinforce this interpretation, hewrote (i /∂ − m)ψ = 0 asi ∂ψ∂t = −i⃗α · ⃗∇ψ + mβψ ≡ Ĥψ (5.22)where ⃗α = −γ 0 ⃗γ and β = γ 0 . Here the operator Ĥ is interpreted as the one-particleHamiltonian. This is a very different viewpoint from the one we now have, where ψis a classical field that should be quantized. In Dirac’s view, the Hamiltonian of thesystem is Ĥ defined above, while for us the Hamiltonian is the field operator (5.17).Let’s see where Dirac’s viewpoint leads.With the interpretation of ψ as a single-particle wavefunction, the plane-wave solutions(4.104) and (4.110) to the Dirac equation are thought of as energy eigenstates,withψ = u(⃗p) e −ip·x ⇒ i ∂ψ∂t = E ⃗p ψψ = v(⃗p) e +ip·x ⇒ i ∂ψ∂t = −E ⃗p ψ (5.23)which look like positive and negative energy solutions. The spectrum is once againunbounded below; there are states v(⃗p) with arbitrarily low energy −E ⃗p . At firstglance this is disastrous, just like the unbounded field theory Hamiltonian (5.12). Diracpostulated an ingenious solution to this problem: since the electrons are fermions (afact which is put in by hand to Dirac’s theory) they obey the Pauli-exclusion principle.So we could simply stipulate that in the true vacuum of the universe, all the negativeenergy states are filled. Only the positive energy states are accessible. These fillednegative energy states are referred to as the Dirac sea. Although you might worry aboutthe infinite negative charge of the vacuum, Dirac argued that only charge differenceswould be observable (a trick reminiscent of the normal ordering prescription we usedfor field operators).Having avoided disaster by floating on an infinite sea comprised of occupied negativeenergy states, Dirac realized that his theory made a shocking prediction. Suppose thata negative energy state is excited to a positive energy state, leaving behind a hole.The hole would have all the properties of the electron, except it would carry positivecharge. After flirting with the idea that it may be the proton, Dirac finally concludedthat the hole is a new particle: the positron. Moreover, when a positron comes across– 111 –
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4.7.2 Some Useful Formulae: Inner a
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0. Introduction“There are no real
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At distances shorter than this, the
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which allows us to express all dime
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1. Classical Field TheoryIn this fi
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and the potential energy of the fie
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1.2 Lorentz InvarianceThe laws of N
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Example 3: Maxwell’s EquationsUnd
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(where the sign in the field transf
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from which we see thatδφ = −ω
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Another Cute TrickThere is a quick
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2. Free Fields“The career of a yo
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Substituting into the above express
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Hmmmm. We’ve found a delta-functi
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2.3.2 The Casimir Effect“I mentio
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This is still infinite in the limit
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This space is known as a Fock space
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From this result we can figure out
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2.6 The Heisenberg PictureAlthough
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But what about arbitrary spacetime
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where T stands for time ordering, p
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Im(p 0)Im(p 0)−E p+ E pRe(p 0)−
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We may expand ψ(⃗x) as a Fourier
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which confirms (2.120). So we learn
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3. Interacting FieldsThe free field
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The interaction picture is a hybrid
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Actually these last two terms doubl
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• Obviously we can’t cope with
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where the ± signs on φ ± make li
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