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7.6

Fermi's golden rule

When the final states form a continuum, the oscillating transition probability becomes a constant transition rate — one formula that rules every calculation of emission, absorption and scattering.

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After this section you should be able to

  • Explain why a continuum of final states turns t² growth and oscillation into a constant rate
  • Complete the derivation of the golden rule, making clear how sinc² becomes an energy-conserving δ function in the long-time limit
  • Recast the pair of factors "energy conservation + how many places to go" in the language of the density of states
  • Estimate the order of magnitude of the hydrogen 2p→1s spontaneous-emission lifetime (nanoseconds), and state the golden rule's window of validity in time

The last section left a crack. For a single final state, first-order theory gives a probability that either grows madly as t2t^2 (on resonance) or oscillates back and forth (off resonance). Yet excited atoms in the laboratory wear an entirely different face: a population of hydrogen atoms in the 2p state loses a fixed fraction every nanosecond, its number sliding smoothly down as et/τ\ee^{-t/\tau} with τ=1.6 ns\tau=1.6\ \text{ns} — no oscillation, no acceleration. “A fixed fraction per unit time” means there exists a constant transition rate Γ\Gamma. Where does this constant rate spring from?

The difference hides in the nature of the final states. Last section we tacitly assumed the transition’s destination was one discrete state; but when an atom emits light, the destination is “the atom drops to 1s plus a photon flies away” — and the photon can fly in any direction, carry either of two polarisations, and take any frequency within the resonance width. The final state is not a point; it is a continuum. When we measure “has the atom decayed yet?”, we do not care which way the photon went, so the probability must be summed over the whole continuum. It is this summation that flattens the oscillations into a rate.

Counting the final states: the density of states

To sum over a continuum, we first need to answer “how many states are there per unit energy interval near EE?” That quantity is the density of states, written ρ(E)\rho(E): there are ρ(E)dE\rho(E)\,\dd E states with energy between EE and E+dEE+\dd E. It is a pure counting problem, with no dynamics in it.

The most common example: a particle (or photon) placed in a large box of volume V=L3V=L^3, with momentum quantised onto the lattice k=2πL(nx,ny,nz)\vec k=\frac{2\pi}{L}(n_x,n_y,n_z). Each state occupies a volume (2π/L)3(2\pi/L)^3 of kk-space; count the lattice points in a spherical shell of radius kk, convert to energy, and out comes ρ(E)\rho(E). For photons (E=ckE=\hbar ck, two polarisations):

ρphoton(E)=VE2π23c3(7.6.1)\rho_{\text{photon}}(E)=\frac{V E^2}{\pi^2\hbar^3c^3}\tag{7.6.1}

The box is only scaffolding: in any physical answer, VV always cancels against the 1/V1/V normalisation factor in the matrix element, and the final rate is independent of the box size.

From sinc² to a rate

An order-of-magnitude calculation: why the atom lives 1.6 nanoseconds

The golden rule’s most famous client: spontaneous emission. A hydrogen atom falls from 2p back to 1s, releasing a 10.2 eV photon. The matrix element comes from the electric-dipole interaction (V^erE\hat V\sim e\vec r\cdot\vec{\mathcal E}, dipole moment of order ea0ea_0); the density of states is the photon formula above. Feed both into the golden rule, sum over photon directions and polarisations, and the rate tidies up to

Γ4α3ω3a02c2×matrix element/ea02(7.6.10)\Gamma\approx\frac{4\alpha}{3}\,\frac{\omega^3a_0^2}{c^2}\times|\text{matrix element}/ea_0|^2\tag{7.6.10}

(α1/137\alpha\approx1/137 is the fine-structure constant.) The arithmetic: ω=1.55×1016 rad/s\omega=1.55\times10^{16}\ \text{rad/s}, taking the matrix-element factor as 1 for now:

Γ43×137×(1.55×1016)3×(5.29×1011)2(3×108)21.1×109 s1(7.6.11)\Gamma\approx\frac{4}{3\times137}\times\frac{(1.55\times10^{16})^3\times(5.29\times10^{-11})^2}{(3\times10^8)^2} \approx1.1\times10^{9}\ \text{s}^{-1}\tag{7.6.11}

The exact matrix element 1sz2p0=0.745a0|\bra{1s}z\ket{2p_0}|=0.745\,a_0 squeezes in a further factor of 0.55, giving Γ=6.3×108 s1\Gamma=6.3\times10^8\ \text{s}^{-1}, i.e.

τ=1Γ1.6 ns(7.6.12)\tau=\frac{1}{\Gamma}\approx1.6\ \text{ns}\tag{7.6.12}

in exact agreement with experiment. Take a moment to feel what this number means: the light wave’s period is 2π/ω0.4 fs2\pi/\omega\sim0.4\ \text{fs}, so the atom oscillates through four million periods before emitting one photon — the coupling of atom to light field (powers of α\alpha) is genuinely feeble, which in turn explains why first-order perturbation theory is so trustworthy here.

Push the same rule outward and you get the whole of spectroscopy and scattering physics: photoabsorption cross-sections, beta-decay rates (Fermi’s own use for it), electron–phonon scattering in solids, the resistance of metals — for any problem where “an initial state flows through a weak coupling into a continuum of final states”, step one is always to write down the golden rule.

What comes next

Time-dependent perturbation theory handles disturbances that are “fast but weak”: the light field oscillates millions of periods before triggering a single transition. Now twist the dial to the opposite end — what if the disturbance is extremely slow? Compress the well gradually, rotate the magnetic field gently: will the system jump away, or follow along obediently? The answer (the adiabatic theorem) is useful in its own right, but in 1984 Berry discovered a character in the story that had been overlooked for half a century: a system carried slowly around a closed loop comes back with a phase imprinted on its wavefunction that depends only on the geometry of the path. This “geometric phase” went on to thread together the Aharonov–Bohm effect and the entire field of topological matter.

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