A model its own author admitted was an unprincipled patchwork — and it gave the hydrogen spectrum to four significant figures. Both what it got right and what it got wrong are worth seeing clearly.
✓Derive the hydrogen energy levels and the Rydberg formula from Bohr's two postulates
✓Compute the Bohr radius and 13.6 eV, and identify which constants they are built from
✓State the correspondence principle and show how Bohr used it to reverse-engineer the quantisation condition
✓Name three kinds of phenomena the model cannot handle
The previous section left the third dead end standing: a classical atom lives under 10−11 s and ought to emit a continuous spectrum.
Start by looking at what experiment actually offered.
Spectral lines are not random — they have a formula
Nineteenth-century spectroscopy accumulated a great deal of data: each element, heated or discharged, emits only at certain wavelengths, fixed precisely enough to identify the element.
Hydrogen is the simplest, with only a handful of visible lines. In 1885 Balmer, a Swiss schoolteacher of mathematics, stared at those four numbers and found a formula. Rydberg later generalised it:
λ1=R∞(n121−n221),n2>n1(1.4.1)
with R∞=1.097×107m−1 fitted purely from experiment.
Bohr’s two postulates
In 1913 Bohr proposed two postulates in direct conflict with classical physics. He knew perfectly well they were unjustified; the plan was to accept them and see what followed.
The first postulate cuts off the collapse directly: an electron in a stationary state does not radiate, so it cannot spiral in; and n=1 is the lowest rung, with no step below it, so the atom is stable.
The second turns the “difference of two terms” in the Rydberg formula into “difference of two energy levels”.
Derivation: from two postulates to 13.6 eVbasic~8 minexpand
Step 1: classical mechanics gives the orbit condition. The Coulomb force supplies the centripetal force:
4πε0r2e2=rmv2⟹mv2=4πε0re2(1.4.4)
Note this step is entirely classical — Bohr invoked quantum assumptions only where he had to, and used Newton everywhere else.
Step 2: impose the quantisation condition. From mvr=nℏ we get v=nℏ/mr; substituting,
m⋅m2r2n2ℏ2=4πε0re2⟹rn=me24πε0ℏ2n2(1.4.5)
The orbital radii are discrete and go as n2. The smallest (n=1) is the Bohr radius:
a0=me24πε0ℏ2=0.529A˚=5.29×10−11m(1.4.6)
This matched the atomic size then estimated from gas viscosity and similar methods. A length assembled purely from fundamental constants landing at the right order of magnitude — this was the model’s first genuinely persuasive moment.
Step 3: compute the energy. Total energy is kinetic plus potential:
(using step 1’s mv2=e2/4πε0r; note in passing that the kinetic energy is exactly half the magnitude of the potential energy, a consequence of the virial theorem for a Coulomb force).
Substituting rn:
En=−32π2ε02ℏ2me4⋅n21=−n213.606eV(1.4.8)
Step 4: match the Rydberg formula. By postulate two,
hν=En2−En1=13.606eV(n121−n221)(1.4.9)
In terms of wavelength,
λ1=hc13.606eV(n121−n221)(1.4.10)
That leading coefficient works out to 1.097×107m−1 — agreeing with the measured Rydberg constant to four significant figures.
Thirty years of numerical puzzle, solved.
◑The picture
What the level diagram looks like
En=−13.6/n2 eV: −13.6,−3.40,−1.51,−0.85,…
The gaps shrink as you climb, crowding towards E=0 (where the electron just escapes). So:
Transitions down to n1=1 (the Lyman series) carry the most energy and lie in the ultraviolet.
Down to n1=2 (the Balmer series) happen to land in the visible — these are the four lines Balmer could see with his eyes.
Down to n1=3 (the Paschen series) lie in the infrared.
∑The mathematics
En=−n213.606eV,rn=a0n2(1.4.11)
The ionisation energy — taking the electron from n=1 to n=∞ — is 13.6 eV, in exact agreement with experiment.
Using the fine-structure constant α=e2/4πε0ℏc≈1/137 it can be written very cleanly:
En=−21α2mc2⋅n21(1.4.12)
that is, 21×(1/137)2×511000eV=13.6eV.
The correspondence principle: how Bohr found that condition
In the derivation above, L=nℏ was written down out of nowhere. Bohr did not guess it — he had a methodological principle.
Check: the two frequencies really do agree at large nadvanced~6 minexpand
Quantum side. The gap between adjacent levels:
ΔE=En+1−En=13.6eV(n21−(n+1)21)(1.4.13)
Expanding for large n: n21−(n+1)21≈n32, so
νquantum=hΔE≈hn32×13.6eV(1.4.14)
Classical side. The orbital frequency is f=v/2πr. With v=nℏ/mr and r=a0n2:
Both go as 1/n3, and putting the constants in shows the coefficients match too.
For a feel for the numbers: at n=2→1 the two differ by more than a factor of two; at n=100→99 by under 2%; at n=1000 they are indistinguishable.
Quantum effects do not “vanish” at large n; they simply become impossible to tell apart from the classical answer. The same idea reappears in another guise in section 2.7.
Where it goes wrong
The Bohr model is absurdly accurate for hydrogen, but it is a semi-classical patchwork: half Newtonian orbit, half quantum rule, and the two are fundamentally incompatible.
∎Key formulas
Angular-momentum quantisation
L=mvr=nℏ,n=1,2,3,…
Bohr's first postulate, reverse-engineered from the correspondence principle
Bohr radius
a0=me24πε0ℏ2=0.529A˚
An atomic scale assembled purely from fundamental constants
Hydrogen energy levels
En=−n213.606eV=−2n2α2mc2
The levels themselves are right; quantum mechanics re-derives them
Rydberg formula
λ1=R∞(n121−n221)
R∞ = 1.097×10⁷ m⁻¹; theory and experiment agree to four figures
?Self-check4 questions
1.
How does the Bohr model deal with "an atom collapses within 10⁻¹¹ s"?
2.
What role does the correspondence principle play in Bohr's work?
3.
Which statements about the limitations of the Bohr model are correct? (Select all that apply.)
Select all that apply
4.
What is the photon energy, in eV, for the hydrogen transition n = 3 → n = 2? (This is the Balmer Hα line, and it is red.)
eV10% relative tolerance
What comes next
Bohr’s quantisation condition L=nℏ is still a rule with no reason behind it. Why integer multiples of ℏ in particular?
Ten years later a doctoral student gave an unexpected answer: because the electron is a wave, and the orbit has to hold a whole number of wavelengths.