
Advanced Quantum Mechanics course sequence · Interactive lesson
Magnetic-dipole emission and the 21 cm rate computed
Radio astronomers map the Galaxy with a line whose upper level lives eleven million years, a number Quantum Mechanics II could only quote. Here we compute it: topic 12.02's mode sum run again with the spin coupled to the quantised B field, the reason magnetic lines are slow, and why in space the background light does most of the emitting.
UAQM-12.04 · Lesson 4 of 9 in this unit. Position is not a completion score.Build the model
Couple the spin to the vacuum's B field and the 21 cm level lives eleven million years.
The key idea
Magnetic-dipole emission is spontaneous decay driven by the coupling −μ⋅B of an atom's magnetic moment to the vacuum fluctuations of the quantised magnetic field, at the rate μ₀ω³|⟨f|μ|i⟩|²/(3πħc³).
Example. Hydrogen's hyperfine flip at 1420.406 MHz has |⟨f|μ|i⟩| = μB, so A = 2.87 × 10⁻¹⁵ s⁻¹ and the upper level lives 3.49 × 10¹⁴ s, or 11.0 million years, against 1.6 ns for hydrogen's 2p level.
The complete physical model and assumptions
Unit 11's atom-field Hamiltonian holds a second first-order coupling beside A⋅p: the spin term −μ⋅B. Once B = ∇ × A is quantised, every mode carries a vacuum magnetic field of amplitude √(μ₀ħω/2V), its electric amplitude divided by c, and the a† inside it lets an excited atom emit into empty modes as in topic 12.02. The magnetic polarisation vectors k̂ × ε are the electric pair turned through 90° about k, so the polarisation sum, the 8π/3 of the angular integral and the cancelling volume all carry over, and the magnetic-dipole rate is A = μ₀ω³|⟨f|μ|i⟩|²/(3πħc³), derived. At equal frequency that is |μ|²/(c²|d|²) of an electric-dipole rate, and because μB/(e a₀ c) is exactly α/2, a one-magneton moment radiates (α/2)² = 1.3 × 10⁻⁵ as fast as an e a₀ dipole. Hydrogen's F = 1 → F = 0 flip is the clean case: the electron spin carries a full μB between the two hyperfine states, the measured 1420.406 MHz fixes ω, and A = 2.87 × 10⁻¹⁵ s⁻¹ follows, a lifetime of 11.0 million years. The model stops where its operator does. μ = −μB(L + 2S)/ħ never touches the radial coordinate, so without relativity it links only partners inside one fine- or hyperfine-structure multiplet, and it is first order with e(ik⋅r) set to 1. In space the rate is not the whole story: the 2.725 K background puts 39.5 photons into each 1420 MHz mode, and stimulated emission outruns spontaneous by that factor.
1The spin term with a quantised magnetic field
Units are SI throughout, and the atom moves slowly, so no four-vectors and no metric signature enter. Unit 11 ordered the atom-field Hamiltonian in powers of e; at first order it holds (e/m)A⋅p and the spin term −μ⋅B. Take the curl of the quantised A: each mode contributes a magnetic field of amplitude √(ħ/2ε₀ωV) × ω/c = √(μ₀ħω/2V), directed along k̂ × ε. Emission into an empty mode uses the a† term, whose √(n + 1) is 1, so ⟨f, 1|−μ⋅B|i, 0⟩ has magnitude √(μ₀ħω/2V)|⟨f|μ|i⟩⋅(k̂ × ε)|. The orbital moment comes out of A⋅p at first order in k⋅r: (k⋅r)(ε⋅p) = ½[(k⋅r)(ε⋅p) + (ε⋅r)(k⋅p)] + ½(k × ε)⋅L, and the last piece is exactly −μL⋅B with μL = −μB L/ħ. Spin and orbit join in μ = −μB(L + 2S)/ħ, the 2 being the Dirac equation's; the symmetric piece is the electric quadrupole. The spin term itself needs only e(ik⋅r) ≈ 1, and for 21 cm ka₀ = 1.6 × 10⁻⁹.
2The mode sum, run a second time
Topic 12.02's machinery now applies unchanged. For a right-handed triad (ε₁, ε₂, k̂), k̂ × ε₁ = ε₂ and k̂ × ε₂ = −ε₁: the magnetic polarisation vectors are the electric pair turned through 90°, still orthonormal and perpendicular to k. So Σλ|μfi⋅(k̂ × ελ)|² = |μfi|² − |k̂⋅μfi|², whose integral over directions is (8π/3)|μfi|². With Vω²/(8π³c³) modes per unit ω and solid angle, the golden rule gives A = (2π/ħ²)(Vω²/8π³c³)(μ₀ħω/2V)(8π/3)|μfi|² = μ₀ω³|μfi|²/(3πħc³), derived, with V cancelling: topic 12.02's result with d replaced by μ/c. Classical limit: a moment m₀ cos ωt radiates μ₀ω⁴m₀²/(12πc³), quoted from electromagnetism, and with m₀ = 2|μfi| that power divided by ħω is the same rate. A Δm = 0 line again has the sin²θ pattern, but its electric vector lies along μ × k̂, turned 90° from the electric-dipole case: polarisation, not angular shape, tells M1 from E1.
3Why magnetic lines are slow, and where they live
Divide the two rates at one frequency: AM1/AE1 = |μfi|²/(c²|dfi|²). The atomic sizes are μB = eħ/2mₑ and e a₀, and since a₀ = ħ/(mₑcα), μB/(e a₀ c) = α/2 exactly, so a one-magneton moment radiates (α/2)² = 1.33 × 10⁻⁵ as fast as an e a₀ dipole. The reason is kinematic: a charge e circling at radius r and speed v has μ = evr/2 and d = er, so μ/(cd) = v/2c, and Bohr's orbit has v = αc. Selection rules then put M1 lines where ω³ hurts most. μ is an axial vector, even under parity, so it links states of equal parity, exactly where electric-dipole decay is forbidden; and −μB(L + 2S)/ħ never touches the radial coordinate, so without relativity it connects only states sharing a radial function: members of one fine- or hyperfine-structure multiplet, with ΔJ or ΔF = 0, ±1 and 0 → 0 excluded. Those splittings are small. Hydrogen's 1s and 2s radial functions are orthogonal, so ⟨1s|μ|2s⟩ = 0; relativistic corrections give the 2s a magnetic rate of 2.5 × 10⁻⁶ s⁻¹, quoted, far below its two-photon rate of 8.2 s⁻¹.
4The hyperfine transition moment from coupled spins
Quantum Mechanics II built hydrogen's ground hyperfine states from the two spins, quoted here with ↑ for the electron and ⇑ for the proton: |1, 1⟩ = |↑⇑⟩, |1, 0⟩ = (|↑⇓⟩ + |↓⇑⟩)/√2 and |0, 0⟩ = (|↑⇓⟩ − |↓⇑⟩)/√2. Both are 1s, so L = 0 and the moment is the spins': μ = −μB σₑ + (gₚ/2)μN σₚ, with gₑ = 2. The z component of σₑ turns |1, 0⟩ into (|↑⇓⟩ − |↓⇑⟩)/√2 = |0, 0⟩, so the electron gives ⟨0, 0|μz|1, 0⟩ = −μB. From |1, 1⟩ the x and y components of σₑ give |↓⇑⟩ and i|↓⇑⟩, each of magnitude 1/√2 on |0, 0⟩, so the squared moment is ½μB² + ½μB² = μB² again: every substate decays at one rate, as rotational symmetry demands. The proton spin's element is −1 instead of +1, and its charge is opposite, so the two moments add: the amplitude grows by gₚmₑ/2mₚ = 0.15% and the rate by 0.30%. For a nucleus of spin I the same steps from the stretched state |↑, mI = I⟩ give Σ|⟨f|σₑ|i⟩|² = 4I/(2I + 1), which is 1 for the proton.
5Eleven million years, computed and checked
The measured 1420.405752 MHz gives ω = 8.925 × 10⁹ rad s⁻¹ and ω³ = 7.108 × 10²⁹ s⁻³. With μ₀μB²/(3πħc³) = 4.036 × 10⁻⁴⁵ s², A₁₀ = 2.869 × 10⁻¹⁵ s⁻¹ and τ = 3.49 × 10¹⁴ s = 11.0 million years: the 2.9 × 10⁻¹⁵ s⁻¹ Quantum Mechanics II quoted, now derived. The proton's moment and gₑ = 2.00232 raise it to 2.884 × 10⁻¹⁵ s⁻¹, the value radio astronomy uses. The natural width A₁₀/2π = 4.6 × 10⁻¹⁶ Hz is invisible beside a 10 kHz Doppler width at 100 K. No laboratory can wait eleven million years, but hydrogen-like ²⁰⁹Bi⁸²⁺, with I = 9/2, has the same transition at 243.87 nm, and its lifetime was measured in a storage ring as 0.397 ± 0.016 ms. Scale from hydrogen: the frequency ratio cubed is 6.48 × 10¹⁷ and 4I/(2I + 1) = 1.8, giving 0.299 ms. At Z = 83 the bound electron's g is 1.728, Breit's Dirac-equation result, quoted, and (g/2)² = 0.746 lengthens the estimate to 0.400 ms, inside the error bar.
6In space the background does most of the emitting
Interstellar hydrogen does not sit in empty space. At 2.725 K, hν/kT = 0.0682 K/2.725 K = 0.0250, so each 1420 MHz mode holds n̄ = 1/(e0.0250 − 1) = 39.5 photons, close to kT/hν − ½. Topic 12.03's rates then apply: an F = 1 atom emits at A₁₀(n̄ + 1) = 1.16 × 10⁻¹³ s⁻¹, stimulated 39.5 times as often as spontaneously, and an F = 0 atom absorbs at 3A₁₀n̄ = 3.40 × 10⁻¹³ s⁻¹, the 3 counting the upper level's substates. With radiation alone the populations relax at A₁₀(4n̄ + 1), in 2.2 × 10¹² s or about 7 × 10⁴ years, to N₁/N₀ = 3e(−hν/kT) = 2.93: the background's own temperature, with emission and absorption cancelling. A 21 cm line seen against the background therefore needs something else to set the populations. In a cloud of one atom per cubic centimetre, spin-exchange collisions at roughly 10⁻¹⁰ s⁻¹ per atom, quoted, outpace the radiative rates and tie the spin temperature to the gas.
Key equations
Read the units, assumptions and limits before substituting.
Vacuum magnetic field of the modes
B = Σ i√(μ₀ħω/2V) (k̂ × ε)[a e(ik⋅r) − a† e(−ik⋅r)]
The curl of Unit 11's A, derived: each mode's magnetic amplitude is its electric amplitude over c, along ε turned 90° about k.
B in T; μ₀ = 1.257 × 10⁻⁶ N A⁻²; ω in rad s⁻¹; V the box volume in m³; one term per mode k and real polarisation εMagnetic-dipole A coefficient
AM1 = μ₀ω³|⟨f|μ|i⟩|²/(3πħc³)
Derived: golden rule over empty modes, polarisation sum |μ|² − |k̂⋅μ|², angular integral 8π/3, and V cancels. With 1 T = 1 N A⁻¹ m⁻¹ the units reduce to s⁻¹.
ω in rad s⁻¹; |⟨f|μ|i⟩|² in J² T⁻², summed over final substates; ħ in J s; AM1 in s⁻¹Magnetic against electric at one frequency
AM1/AE1 = |μfi|²/(c²|dfi|²) ≈ (α/2)² = 1.33 × 10⁻⁵
Why magnetic lines are slow, derived: a charge e on an orbit of radius r and speed v has μ = evr/2 and d = er, so μ/(cd) = v/2c, and v = αc.
for |μfi| = μB = eħ/2mₑ and |dfi| = e a₀; μB/(e a₀ c) = α/2 exactly, since a₀ = ħ/(mₑcα)Hydrogen's hyperfine transition moment
|⟨F = 0|μ|F = 1, m⟩|² = μB²(1 + gₚmₑ/2mₚ)² for m = −1, 0, +1
Derived from Quantum Mechanics II's coupled spin states. The electron gives μB; the proton adds 0.30% to the rate, and gₑ − 2 another 0.23%.
μ = −μB σₑ + (gₚ/2)μN σₚ with gₑ = 2; gₚ = 5.586; μN = μB mₑ/mₚ; the bracket is 1.0015The 21 cm rate
A₁₀ = μ₀ω³μB²/(3πħc³) = 2.87 × 10⁻¹⁵ s⁻¹
Computed: a lifetime of 3.49 × 10¹⁴ s, or 11.0 million years. Both small corrections together give 2.884 × 10⁻¹⁵ s⁻¹, the value radio astronomy uses.
ω = 2π × 1420.406 MHz = 8.925 × 10⁹ rad s⁻¹ from the measured line; gₑ = 2 and the proton moment neglectedPhotons per 1420 MHz mode in the cosmic background
n̄ = 1/(e(hν/kT) − 1) = 39.5 at T = 2.725 K
Planck's occupation from topic 12.03: stimulated emission runs at A₁₀n̄, 39.5 times the spontaneous rate, and absorption from F = 0 at 3A₁₀n̄.
hν/k = 0.0682 K for ν = 1420.406 MHz; T the measured background temperature; n̄ ≈ kT/hν − ½ when hν ≪ kTInteractive lab
Predict first. Explore the model. Compare the result.
Explore the model
Try this. The default is the 21 cm line: 2.87 × 10⁻¹⁵ s⁻¹, a lifetime of 11.0 million years, with 39.5 background photons per mode lifting the open dot 1.6 decades. Slide to 6.25, at the Lyman α label, and the rate climbs 18.75 decades while n̄ falls to nothing. Halve |μ| and the solid line drops 0.6 decade.
Live results
- log₁₀ M1 RATE / s⁻¹
- -14.54
- log₁₀ LIFETIME / yr
- 7.04
- PHOTONS PER MODE n̄
- 39.5
- E1 / M1 RATE AT EQUAL ω
- 75115
Results follow this lesson’s model and assumptions. Displayed values are rounded.
Predict → change one variable → check
Plan a change before running it. Every other input stays at the saved baseline.
Saved baseline. Frequency log₁₀(ν / 1420 MHz): 0.00; Transition moment |⟨f|μ|i⟩| / μB: 1.00; Background temperature T: 2.725 K
This experiment is kept only while this page is open. It does not change saved course progress.
Catch the common trap
Calling the 21 cm line forbidden invites the conclusion that its matrix element is small. It is not: ⟨F = 0|μ|F = 1⟩ is a full Bohr magneton, as large as one spin's moment can be, and the transition is fully allowed as a magnetic dipole; forbidden only means not electric-dipole. Set against hydrogen's 2p decay, the 21 cm rate is smaller by 4.6 × 10⁻²⁴, and that factor splits into two pieces no selection rule supplies. Being magnetic costs (α/2)², which beside the 2p element |d|² = 0.555 e²a₀² is 2.4 × 10⁻⁵. The frequency, 1.74 × 10⁶ times lower than Lyman-α, costs its cube, 1.9 × 10⁻¹⁹. Their product is the whole factor. Put the same moment at the Lyman-α frequency and it would decay at 1.5 × 10⁴ s⁻¹, in 67 μs: the 21 cm level is long-lived because its splitting is tiny, not because the spin is reluctant to flip.
Practice & worked examples
3 authored examples. Make an attempt, then reveal the reasoning one step at a time.
EasyExample 1
A magnetic-dipole line has |⟨f|μ|i⟩| = μB. At what wavelength would its upper level live 1.0 s against spontaneous emission? Repeat for an electric-dipole line with |d| = e a₀, and compare the two.
Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.
0 of 4 steps revealed.
- Write AM1 = Kω³ with K = μ₀μB²/(3πħc³) = (1.2566 × 10⁻⁶)(9.274 × 10⁻²⁴)²/(3π × 1.0546 × 10⁻³⁴ × (2.998 × 10⁸)³) = 4.04 × 10⁻⁴⁵ s². Units: μ₀μB² is N A⁻² × A² m⁴ = J m³ and ħc³ is J m³ s⁻², so K is in s², as A = Kω³ in s⁻¹ requires.
- τ = 1.0 s means A = 1.0 s⁻¹, so ω = K(−1/3) = 6.28 × 10¹⁴ rad s⁻¹, ν = ω/2π = 1.00 × 10¹⁴ Hz and λ = c/ν = 3.0 μm, in the infrared.
- Check against 21 cm: this frequency is 7.04 × 10⁴ times 1420 MHz, and (7.04 × 10⁴)³ = 3.49 × 10¹⁴, the 21 cm lifetime in seconds, as A ∝ ω³ requires.
- Electric dipole: KE1 = e²a₀²/(3πε₀ħc³) = 3.03 × 10⁻⁴⁰ s², larger by (2/α)² = 7.51 × 10⁴. For A = 1.0 s⁻¹, ω must be lower by the cube root of 7.51 × 10⁴, 42.2: ν = 2.37 × 10¹² Hz and λ = 127 μm.
Answer. λ = 3.0 μm for the magnetic dipole and 127 μm for the electric one: a 1 s lifetime needs a magnetic line 42 times higher in frequency, the cube root of (2/α)² = 7.5 × 10⁴.
MediumExample 2
Deuterium's ground hyperfine line, F = 3/2 → F = 1/2 with nuclear spin I = 1, is measured at 327.384 MHz. Using Quantum Mechanics II's coupled states, written |electron, mI⟩, find Σ|⟨f|σₑ|i⟩|² from |3/2, 1/2⟩, then the spontaneous rate and lifetime, and how much faster stimulated emission runs in the 2.725 K background.
Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.
0 of 5 steps revealed.
- The deuteron's moment, 0.857 μN, is neglected, so |⟨f|μ|i⟩|² = μB²|⟨f|σₑ|i⟩|² with gₑ = 2, summed over both F = 1/2 substates. The states needed are |3/2, 1/2⟩ = √(2/3)|↑, 0⟩ + √(1/3)|↓, 1⟩, |1/2, 1/2⟩ = −√(1/3)|↑, 0⟩ + √(2/3)|↓, 1⟩ and |1/2, −1/2⟩ = −√(2/3)|↑, −1⟩ + √(1/3)|↓, 0⟩.
- The z component of σₑ gives √(2/3)|↑, 0⟩ − √(1/3)|↓, 1⟩, whose overlap with |1/2, 1/2⟩ is −√2/3 − √2/3 = −2√2/3: squared, 8/9.
- The x and y components turn the |↑, 0⟩ part into |↓, 0⟩ and i|↓, 0⟩ (the |↓, 1⟩ part goes to |↑, 1⟩, which has M = 3/2 and no F = 1/2 partner), each with amplitude √(2/3) × √(1/3) = √2/3 on |1/2, −1/2⟩: together 2/9 + 2/9 = 4/9. The sum is 8/9 + 4/9 = 4/3, which is 4I/(2I + 1) at I = 1.
- ω = 2π × 327.384 MHz = 2.057 × 10⁹ rad s⁻¹ and ω³ = 8.704 × 10²⁷ s⁻³, so A = (4/3)(4.036 × 10⁻⁴⁵ s²)(8.704 × 10²⁷ s⁻³) = 4.68 × 10⁻¹⁷ s⁻¹ and τ = 2.14 × 10¹⁶ s = 6.8 × 10⁸ years. Check: hydrogen's 2.869 × 10⁻¹⁵ s⁻¹ times (4/3)(327.384/1420.406)³ = 0.0163 gives the same.
- Background: hν/k = 0.01571 K, so hν/kT = 0.00577 and n̄ = 1/(e0.00577 − 1) = 173. Stimulated emission runs at 173A = 8.1 × 10⁻¹⁵ s⁻¹, and n̄ is 4.4 times hydrogen's 39.5 because n̄ ≈ kT/hν.
Answer. Σ|⟨f|σₑ|i⟩|² = 4/3; A = 4.68 × 10⁻¹⁷ s⁻¹ and τ = 2.14 × 10¹⁶ s, or 6.8 × 10⁸ years; in the 2.725 K background n̄ = 173, so stimulated emission runs 173 times faster than spontaneous.
HardExample 3
Boron-like Ar¹³⁺ has one 2p electron outside closed 1s² and 2s² shells, and its ²P₃/₂ level decays to ²P₁/₂ by emitting at 441.3 nm. Show that the decay is magnetic-dipole, find |⟨f|μ|i⟩|² summed over final substates with gₛ = 2, and compute the lifetime. Compare it with the 9.573 ms measured in an electron-beam ion trap, and find what gₛ = 2.00232 changes.
Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.
0 of 5 steps revealed.
- Both levels belong to one configuration, so they share parity and every electric-dipole element between them vanishes; the closed shells carry no moment. The decay is magnetic-dipole, with μ = −μB(L + 2S)/ħ = −μB(J + S)/ħ for the 2p electron.
- The operator J cannot change the quantum number J, so ⟨J = 1/2|J|J = 3/2⟩ = 0 and only the spin acts: ⟨f|μ|i⟩ = −μB⟨f|S|i⟩/ħ. The orbital part of the moment drops out of this transition.
- Take M = 3/2, which is |mₗ = 1, ↑⟩. Sₓ and Sy give (ħ/2)|1, ↓⟩ and (iħ/2)|1, ↓⟩, and |1, ↓⟩ has amplitude √(2/3) on |J = 1/2, M = 1/2⟩, a Clebsch-Gordan coefficient from Quantum Mechanics II. So Σ|⟨f|S|i⟩|²/ħ² = 2 × ¼ × ⅔ = 1/3 and Σ|⟨f|μ|i⟩|² = μB²/3, the same from every M.
- ω = 2πc/λ = 4.268 × 10¹⁵ rad s⁻¹ and ω³ = 7.777 × 10⁴⁶ s⁻³, so A = (4.036 × 10⁻⁴⁵ s²)(7.777 × 10⁴⁶ s⁻³)/3 = 104.6 s⁻¹ and τ = 9.56 ms. The long-wavelength step holds: ka₀ = 7.5 × 10⁻⁴, and the ion is smaller than a₀.
- The measured 9.573 ms is 0.15% longer. With gₛ = 2.00232 the operator is −μB(J + (gₛ − 1)S)/ħ, which multiplies the rate by (gₛ − 1)² = 1.0046 and shortens τ to 9.51 ms. The close agreement at gₛ = 2 is partly fortunate; precise calculations add relativistic and many-electron corrections beyond this lesson.
Answer. A magnetic-dipole decay with Σ|⟨f|μ|i⟩|² = μB²/3: A = 105 s⁻¹ and τ = 9.56 ms, against 9.573 ms measured; gₛ = 2.00232 shortens the estimate to 9.51 ms.
Quick check
Select an answer and explain it before checking.
Review & continue
Magnetic-dipole emission is spontaneous decay driven by the coupling −μ⋅B of an atom's magnetic moment to the vacuum fluctuations of the quantised magnetic field, at the rate μ₀ω³|⟨f|μ|i⟩|²/(3πħc³).
- Explain the relationship without looking at the equation.
- Check a sign, a unit and a model assumption in your working.
- Return to the lab or worked example if a step is still unclear.