The Blackbody Problem & Planck's Quantum Hypothesis
Every course in this site's own Science Subject so far has treated classical physics as reliable ground. This course opens with the exact real moment classical physics genuinely, provably broke — and the reluctant, half-hearted fix that accidentally launched an entirely new branch of physics.
The Ultraviolet Catastrophe
A "blackbody" is an idealised object that absorbs and re-emits all radiation striking it. Late-19th-century physicists tried to predict the real spectrum of light such an object would emit at a given temperature, using established classical physics — the Rayleigh-Jeans law. The result was a genuine, serious problem: the classical formula predicted that radiated energy should keep increasing without limit as frequency rose, implying a real blackbody should radiate an infinite total amount of energy, concentrated at ever-shorter, ultraviolet wavelengths. Real experimental measurements showed nothing of the kind — blackbody radiation genuinely peaks at a specific frequency and falls off afterward. This mismatch, later nicknamed the "ultraviolet catastrophe," was a real, unambiguous sign that something in classical physics itself was fundamentally wrong.
Planck's Real 1900 Solution
Max Planck presented his own real solution to the German Physical Society on 14 December 1900 (building on an earlier version from 19 October the same year). His key, genuinely radical assumption: the oscillators emitting blackbody radiation could not exchange energy continuously, as classical physics assumed, but only in discrete packets, each proportional to the radiation's own frequency:
Here f is frequency and h is a new fundamental constant — now called Planck's constant, with a real measured value of 6.626×10&supminus;³&sup4; J·s. This single assumption, plugged into the math, exactly reproduced the real, observed blackbody spectrum — correctly predicting the falloff at high frequencies that had eluded every purely classical attempt.
Worked Example: The Energy of a Single Photon
What is the energy of a single quantum of green light, with a frequency of roughly 5×10¹&sup4; Hz?
E = (6.626×10&supminus;³&sup4;) × (5×10¹&sup4;)
E ≈ 3.31×10&supminus;¹&sup9; J
This is a genuinely tiny amount of energy on an everyday scale — exactly why the "graininess" of light's own energy went unnoticed for so long, and why classical physics, which treats energy as smoothly continuous, worked so well for ordinary, macroscopic problems right up until it didn't.
Classical Prediction vs. Real, Measured Behaviour
| Property | Classical (Rayleigh-Jeans) | Real, Measured Behaviour |
|---|---|---|
| High-frequency radiation | Increases without limit | Peaks, then falls off |
| Total radiated energy | Predicted infinite | Real, finite, measurable value |
| Energy exchange | Continuous | Discrete, in units of hf |
Hands-On Exercises
Quick Reference
- The ultraviolet catastrophe: classical physics wrongly predicted infinite radiated energy at high frequencies
- Planck's real solution (14 December 1900): energy is exchanged only in discrete packets, E = hf
- Planck's constant: h ≈ 6.626×10&supminus;³&sup4; J·s
- Planck himself originally viewed quantization as a mathematical trick, not physical reality — calling it "an act of despair"