The Crisis of Classical Physics and the Origins of Quantum Mechanics
By 1900 classical physics — Newtonian mechanics, Maxwell's electrodynamics and statistical thermodynamics — described almost everything then measurable. The exceptions were small in number but fatal in kind: the spectrum of thermal radiation, the photoelectric effect, the stability and line spectra of atoms, and the low-temperature behaviour of specific heats. Each is a place where a classical calculation gives a definite, unambiguous answer that experiment flatly contradicts. This chapter follows the historical route by which those anomalies forced the introduction of a single new constant, Planck's , and a single new idea, quantisation, and ends with de Broglie's proposal that matter itself is wavelike — the hypothesis the rest of Unit D turns into a theory.
The organising thread is the quantum of action. Wherever a classical continuum is assumed — a continuous range of oscillator energies, a continuous exchange of energy between light and electrons, a continuous set of orbits — the correct description replaces it with a discrete set, spaced by or . Classical physics is recovered whenever the relevant actions are large compared with ; this is the correspondence principle, and it is the reason the old physics worked so well for so long.
How to read this chapter. Keep three numbers in view: , , and . Every result below is one of these constants tying a particle quantity (energy, momentum) to a wave quantity (frequency, wavelength): , . The "old quantum theory" of Sections 4 and 8 is a scaffold — internally inconsistent, quantitatively right only for the simplest systems — that Chapters 2 and 3 replace with the Schrödinger equation.
1. Blackbody Radiation and the Ultraviolet Catastrophe
A blackbody absorbs all radiation incident on it; in thermal equilibrium at temperature it re-emits with a spectral energy density that depends on and alone, not on the material. Classical physics computes it by counting electromagnetic modes in a cavity — per unit volume per unit frequency — and assigning each the equipartition energy . The result is the Rayleigh–Jeans law,
which matches the data at low frequency and diverges as : the total energy is infinite. This is the ultraviolet catastrophe — not a small discrepancy but a qualitative absurdity.
Planck's resolution (1900). Planck assumed the cavity walls' oscillators of frequency can exchange energy only in integer multiples of . The average energy of an oscillator is then not but
obtained from the Boltzmann-weighted sum over . Multiplying by the mode density gives the Planck law
For the exponential expands to and Planck reduces to Rayleigh–Jeans; for the factor cuts the spectrum off exponentially, curing the catastrophe. Fitting the curve to data fixed for the first time.
Worked example — Wien and Stefan–Boltzmann as corollaries. Maximising gives (Wien's displacement law; in wavelength, ). Integrating over all gives a total energy density , hence a radiated power per unit area with — the Stefan–Boltzmann constant, now expressed through .
2. The Photoelectric Effect
Light striking a clean metal surface ejects electrons. The classical wave picture predicts that the electron energy should grow with intensity and that there should be a measurable delay at low intensity while energy accumulates. Experiment (Lenard, then Millikan) shows the opposite:
- there is a threshold frequency below which no electrons are emitted, at any intensity;
- above threshold the maximum kinetic energy is linear in frequency and independent of intensity;
- the emission is instantaneous (within );
- intensity controls only the number of electrons, not their energy.
Einstein's photon hypothesis (1905). Light of frequency consists of quanta each carrying energy . One quantum is absorbed by one electron; if exceeds the work function (the minimum energy to free an electron from the metal), the electron escapes with
The threshold is ; the slope of versus is , the same as in the Planck law. Millikan's precision measurement of that slope (1916), undertaken to disprove the idea, instead confirmed it and gave an independent value of .
3. The Compton Effect
When X-rays of wavelength scatter from (effectively free) electrons, the scattered radiation contains a component at a longer wavelength that depends on the scattering angle but not on the target material:
The quantity is the Compton wavelength of the electron. The derivation treats the photon as a relativistic particle with energy and momentum , and applies conservation of energy and momentum to a two-body elastic collision. A classical wave, which would drive the electron and be re-radiated at the same frequency, cannot produce a wavelength shift at all. Compton scattering (1923) is the cleanest single demonstration that electromagnetic radiation carries quantised momentum as well as quantised energy.
Worked example — maximum shift and the backscatter peak. The shift is largest at (photon reversed), where . For photons this is a large fractional change and the recoil electron takes most of the energy; for visible light () the same absolute shift is one part in and utterly negligible — which is why the effect was invisible until X-rays.
4. Atomic Spectra and the Bohr Model
Atoms emit and absorb light only at sharp, discrete wavelengths. For hydrogen the wavenumbers fit the Rydberg formula
with positive integers. Classically an orbiting electron radiates continuously, spiralling into the nucleus in about : classical atoms are neither stable nor line-emitting.
Bohr's postulates (1913).
- The electron occupies only certain stationary states, in which — contrary to electrodynamics — it does not radiate.
- The allowed orbits are those for which the angular momentum is quantised: .
- Radiation is emitted or absorbed only in transitions between stationary states, with photon energy .
Applying to a circular Coulomb orbit gives the radii with the Bohr radius , and the energies
The transition rule then reproduces the Rydberg formula and predicts from fundamental constants. The model also fits singly ionised helium (with scaling) but fails for any two-electron system and says nothing about line intensities or splittings.
5. The de Broglie Hypothesis
If light — historically a wave — has particle properties , , then de Broglie (1924) proposed the symmetric statement: a particle of momentum has an associated wavelength
and a frequency . For a non-relativistic particle . This immediately explains Bohr's quantisation condition: a standing wave on the circular orbit requires the circumference to be an integer number of wavelengths, , i.e. . The mysterious postulate becomes a resonance condition.
Worked example — when is the wavelength observable? An electron accelerated through has and — comparable to atomic spacings in a crystal, so diffraction is observable. A bead moving at has , some times smaller than a nucleus: no apparatus can resolve it, and the bead is classical.
6. Matter-Wave Diffraction: the Experimental Confirmation
Davisson and Germer (1927) scattered low-energy electrons from a nickel single crystal and found intensity maxima at exactly the angles predicted by the Bragg condition using the de Broglie . Independently, G. P. Thomson passed electrons through thin polycrystalline films and photographed Debye–Scherrer rings identical in form to X-ray powder patterns. Later experiments extended matter-wave diffraction to helium atoms, neutrons, and molecules as large as fullerenes and beyond. The single-particle double slit — electrons sent through one at a time — builds an interference pattern dot by dot: each electron arrives as a localised event, yet the accumulated distribution is the wave pattern. Wave and particle aspects are both necessary and never observed in the same measurement.
7. Further Cracks: Specific Heats and the Franck–Hertz Experiment
Specific heat of solids. The classical Dulong–Petit law gives a molar heat capacity , temperature-independent. Measurements show as . Einstein (1907) modelled the solid as oscillators each quantised in units of ; the same formula as in the Planck law gives exponentially at low . Debye (1912) improved the low- behaviour to the observed by quantising a spectrum of lattice modes. Either way, quantisation is what freezes out degrees of freedom.
Franck–Hertz (1914). Electrons accelerated through mercury vapour lose energy in fixed lumps of , and the vapour then emits ultraviolet light at exactly the corresponding wavelength. This is a direct, non-spectroscopic demonstration that atomic internal energy is quantised: the collision is inelastic only when the electron can deliver the precise excitation energy.
8. What the Old Quantum Theory Could and Could Not Do
The Bohr–Sommerfeld programme — quantise the action for each periodic coordinate — extended Bohr's model to elliptical orbits and gave the fine structure of hydrogen to leading order. But it is a patchwork:
- it applies only to systems whose classical motion is multiply periodic, i.e. essentially one-body problems with special symmetry;
- it cannot treat the ground state of helium, the hydrogen molecule ion, or any non-separable system;
- it gives energies but not transition rates or selection rules, which have to be grafted on by a correspondence argument;
- it retains classical trajectories, which the uncertainty principle (Chapter 5) will show cannot exist.
What survives into the real theory is the physical core: energy levels are discrete, transitions are quantum jumps with , angular momentum comes in units of , and every particle has a wave associated with it. The task of Chapters 2–4 is to find the equation that wave obeys and the rules for extracting predictions from it.
9. Common Pitfalls
- Calling the photoelectric work function an ionisation energy. is the energy to remove an electron from a metal surface to just outside it; it is a bulk property, typically –, not the ionisation energy of an isolated atom.
- Thinking higher intensity means higher photon energy. Intensity is photons per second times ; the energy per photon is set by frequency alone. A bright red lamp will never eject electrons that a dim blue one can.
- Using the non-relativistic for fast electrons. For fast electrons use the relativistic in ; the non-relativistic is only a low-energy approximation.
- Treating the Compton shift as fractional. is an absolute shift, the same in picometres for X-rays and for visible light; it is only detectable when it is a decent fraction of .
- Believing the Bohr model "explains" the atom. It gets hydrogen's energy levels right by a lucky cancellation and fails for everything else; its orbits are not real. Use it as mnemonic, not mechanism.
- Saying an electron is "sometimes a wave and sometimes a particle." In any single experiment it shows one aspect; the wavefunction (next chapter) is a single object that carries both, with giving the probability of a particle-like detection.
- Forgetting the correspondence limit. Quantum results must reduce to classical ones for large quantum numbers / large actions; if a formula does not, it is wrong.
Summary
- Planck: cavity oscillators have , giving ; reduces to Rayleigh–Jeans for , cuts off exponentially for . Yields Wien ( const) and Stefan–Boltzmann ().
- Photoelectric effect: ; threshold ; energy independent of intensity, emission instantaneous — light delivers energy in quanta .
- Compton effect: , from photon–electron relativistic two-body kinematics with .
- Bohr model: , ; reproduces the Rydberg formula and predicts .
- de Broglie: ; standing-wave condition on a Bohr orbit gives . Confirmed by Davisson–Germer and G. P. Thomson electron diffraction, and by single-particle double-slit build-up.
- Other evidence: specific heats at low (Einstein/Debye); Franck–Hertz shows discrete atomic excitation energies.
- Old quantum theory () works only for multiply periodic one-body systems and gives no transition rates; the surviving physical core is discreteness, quantum jumps, -quantised angular momentum, and universal wave–particle duality.