Exercise 1: Blackbody radiation: Wien, Stefan and the birth of the quantum
Every hot body radiates. The maximum emission occurs at the wavelength given by Wien's law, m·K, and the power radiated per unit area follows the Stefan-Boltzmann law, with W/(m²·K⁴). It was in trying to explain these two laws that Planck was forced, in 1900, to introduce the quantum. The diagram below shows the regions of the spectrum.
- a) Calculate the wavelength of maximum emission of the Sun (surface at 5800 K) and of the human body (310 K). Place each in the spectrum and comment on the coincidence with the sensitivity of the eye.
- b) The filament of an incandescent bulb reaches 2500 K. Calculate its maximum emission and explain why this type of bulb has such a poor luminous efficiency.
- c) Estimate the NET power radiated by an unclothed person with a surface area of 1.8 m², at 306 K, in a room at 293 K. Comment on the order of magnitude.
- d) Classical theory predicted that the radiated energy grows without limit as the wavelength decreases, which came to be called the ultraviolet catastrophe. Explain where this absurd prediction came from and how Planck's hypothesis removes it.
- e) A star has a surface temperature twice that of the Sun. What happens to its maximum emission and to its power per square metre? Why is a red ember cooler than a white-hot piece of metal?
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Answers
- a) nm for the Sun, µm for the body: the eye adjusted to the solar maximum
- b) µm, in the infrared: luminous efficiency of about
- c) W
- d) High-frequency modes are FROZEN: the first quantum exceeds
- e) halved, power multiplied by
Sun: m, that is 500 nm, right in the middle of the visible range, in the green. Human body: m, that is 9.3 μm, in the long-wave infrared, completely invisible to the eye but perfectly picked up by a thermal camera. The coincidence between the solar maximum and the peak sensitivity of the eye, around 555 nm, is of course no coincidence: the eye evolved under this light and adjusted to what was most abundant.
m, that is 1.16 μm: the maximum falls in the INFRARED, outside the visible range. An incandescent bulb therefore emits most of its radiation as invisible heat, and only the short-wavelength tail of its distribution reaches the visible; its luminous efficiency tops out around 5%. To do better, the temperature would have to go up, but tungsten melts at 3695 K: blackbody physics doomed the filament bulb long before regulations got involved.
W. About 140 W, more than the basal metabolic rate of an adult at rest, which explains why we cool down so quickly when unclothed, even in a room at 20 °C. The net power is proportional to the DIFFERENCE of the fourth powers, never to the difference of the temperatures: this is why a gap of only 13 degrees is enough to carry away that much energy. Clothing does not work by suppressing this radiation but by placing an intermediate surface in the way, colder on its outer side.
Classical physics treated the radiation as a set of oscillation modes in a cavity, and the equipartition theorem gave each one the same average energy . But the number of modes grows without limit as the wavelength decreases: the total diverged, and one predicted that an open oven should emit a deadly burst of ultraviolet. Planck assumed that the energy of a mode of frequency can only be , an integer multiple. At high frequencies, the FIRST quantum is already much larger than the typical thermal energy : these modes simply cannot be excited, they stay frozen and stop contributing. The divergence disappears, and the calculated curve matches experiment exactly. Planck regarded this as a mathematical device; it was Einstein who, five years later, made it a physical reality with the photon.
The wavelength of maximum emission is inversely proportional to : it is therefore halved, to 250 nm, in the ultraviolet, and the star looks blue-white since only the edge of its distribution is left to us. The power per square metre goes as : it is multiplied by . The same law ranks the colours of heated objects: a red ember radiates around 1000 K, white-hot iron exceeds 1500 K, and its pale colour signals not a decorative nuance but a maximum emission shifted toward the blue and a power five times greater. In astronomy, the colour of a star is a thermometer.
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