Modern Physicsundergraduate

Planck's Blackbody Radiation Law

Also known as: Planck's law · Planck radiation formula

Heat any object and it glows — dull red, then orange, then white-hot. Classical physics predicted the glow should carry infinite energy at short wavelengths (the 'ultraviolet catastrophe'). Planck fixed it by a desperate guess: light energy comes in discrete lumps hf, not a continuum. That single assumption bends the spectrum back down at short wavelengths and matches every glowing object perfectly. It was the first crack in classical physics and the birth of the quantum.

Bλ(λ,T)=2hc2λ51ehc/λkBT1B_\lambda(\lambda,T)=\frac{2hc^2}{\lambda^5}\,\frac{1}{e^{hc/\lambda k_B T}-1}
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The Planck spectrum reshapes as you change temperature; the peak slides toward shorter wavelengths as T rises.

Equivalent forms

uν=8πhν3c31ehν/kBT1u_\nu=\frac{8\pi h\nu^3}{c^3}\frac{1}{e^{h\nu/k_BT}-1}
One formula spans a campfire, the Sun, and the 2.7 K cosmic microwave background — and it forced h into physics for the first time.