Rayleigh–Jeans law

Comparison of Rayleigh–Jeans law with Wien approximation and Planck's law, for a body of 5800K temperature.

In physics, the Rayleigh–Jeans law is an approximation to the spectral radiance of electromagnetic radiation as a function of wavelength from a black body at a given temperature through classical arguments. For wavelength $\lambda$ , it is:

B_{\lambda }(T)={\frac {2ck_{\mathrm {B} }T}{\lambda ^{4}}},

where

B_{\lambda }

is the spectral radiance, the power emitted per unit emitting area, per steradian, per unit wavelength;

c

is the speed of light;

k_{\mathrm {B} }

is the Boltzmann constant; and

T

is the temperature in kelvins. For frequency

\nu

, the expression is instead

B_{\nu }(T)={\frac {2\nu ^{2}k_{\mathrm {B} }T}{c^{2}}}.

The Rayleigh–Jeans law agrees with experimental results at large wavelengths (low frequencies) but strongly disagrees at short wavelengths (high frequencies). This inconsistency between observations and the predictions of classical physics is commonly known as the ultraviolet catastrophe.^[1]^[2] Its resolution in 1900 with the derivation by Max Planck of Planck's law, which gives the correct radiation at all frequencies, was a foundational aspect of the development of quantum mechanics in the early 20th century.

Historical development[]

In 1900, the British physicist Lord Rayleigh derived the λ⁻⁴ dependence of the Rayleigh–Jeans law based on classical physical arguments and empirical facts.^[1] A more complete derivation, which included the proportionality constant, was presented by Rayleigh and Sir James Jeans in 1905. The Rayleigh–Jeans law revealed an important error in physics theory of the time. The law predicted an energy output that diverges towards infinity as wavelength approaches zero (as frequency tends to infinity). Measurements of the spectral emission of actual black bodies revealed that the emission agreed with the Rayleigh–Jeans law at low frequencies but diverged at high frequencies; reaching a maximum and then falling with frequency, so the total energy emitted is finite.

Comparison to Planck's law[]

In 1900 Max Planck empirically obtained an expression for black-body radiation expressed in terms of wavelength λ = c/ν (Planck's law):

B_{\lambda }(T)={\frac {2hc^{2}}{\lambda ^{5}}}~{\frac {1}{e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}-1}},

where h is the Planck constant and

k B

the Boltzmann constant. The Planck's law does not suffer from an ultraviolet catastrophe, and agrees well with the experimental data, but its full significance (which ultimately led to quantum theory) was only appreciated several years later. Since,

e^{x}=1+x+{x^{2} \over 2!}+{x^{3} \over 3!}+\cdots .

then in the limit of high temperatures or long wavelengths, the term in the exponential becomes small, and the exponential is well approximated with the Taylor polynomial's first-order term,

e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}\approx 1+{\frac {hc}{\lambda k_{\mathrm {B} }T}}.

So,

{\frac {1}{e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}-1}}\approx {\frac {1}{\frac {hc}{\lambda k_{\mathrm {B} }T}}}={\frac {\lambda k_{\mathrm {B} }T}{hc}}.

This results in Planck's blackbody formula reducing to

B_{\lambda }(T)={\frac {2ck_{\mathrm {B} }T}{\lambda ^{4}}},

which is identical to the classically derived Rayleigh–Jeans expression.

The same argument can be applied to the blackbody radiation expressed in terms of frequency ν = c/λ. In the limit of small frequencies, that is $h\nu \ll k_{\mathrm {B} }T$ ,

B_{\nu }(T)={\frac {2h\nu ^{3}}{c^{2}}}{\frac {1}{e^{\frac {h\nu }{k_{\mathrm {B} }T}}-1}}\approx {\frac {2h\nu ^{3}}{c^{2}}}\cdot {\frac {k_{\mathrm {B} }T}{h\nu }}={\frac {2\nu ^{2}k_{\mathrm {B} }T}{c^{2}}}.

This last expression is the Rayleigh–Jeans law in the limit of small frequencies.

Consistency of frequency and wavelength dependent expressions[]

When comparing the frequency and wavelength dependent expressions of the Rayleigh–Jeans law it is important to remember that

{\frac {dP}{d\lambda }}=B_{\lambda }(T),

and

{\frac {dP}{d\nu }}=B_{\nu }(T)

Therefore,

B_{\lambda }(T)\neq B_{\nu }(T)

even after substituting the value

\lambda =c/\nu

, because

B_{\lambda }(T)

has units of energy emitted per unit time per unit area of emitting surface, per unit solid angle, per unit wavelength, whereas

B_{\nu }(T)

has units of energy emitted per unit time per unit area of emitting surface, per unit solid angle, per unit frequency. To be consistent, we must use the equality

B_{\lambda }\,d\lambda =dP=B_{\nu }\,d\nu

where both sides now have units of power (energy emitted per unit time) per unit area of emitting surface, per unit solid angle.

Starting with the Rayleigh–Jeans law in terms of wavelength we get

B_{\lambda }(T)=B_{\nu }(T)\,{\frac {d\nu }{d\lambda }}

where

{\frac {d\nu }{d\lambda }}={\frac {d}{d\lambda }}\left({\frac {c}{\lambda }}\right)=-{\frac {c}{\lambda ^{2}}}.

This leads us to find:

B_{\lambda }(T)={\frac {2k_{\mathrm {B} }T\left({\frac {c}{\lambda }}\right)^{2}}{c^{2}}}\times {\frac {c}{\lambda ^{2}}}={\frac {2ck_{\mathrm {B} }T}{\lambda ^{4}}}.

Other forms of Rayleigh–Jeans law[]

Depending on the application, the Planck function can be expressed in 3 different forms. The first involves energy emitted per unit time per unit area of emitting surface, per unit solid angle, per spectral unit. In this form, the Planck function and associated Rayleigh–Jeans limits are given by

B_{\lambda }(T)={\frac {2hc^{2}}{\lambda ^{5}}}~{\frac {1}{e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}-1}}\approx {\frac {2ck_{\mathrm {B} }T}{\lambda ^{4}}}

or

B_{\nu }(T)={\frac {2h\nu ^{3}}{c^{2}}}{\frac {1}{e^{\frac {h\nu }{k_{\mathrm {B} }T}}-1}}\approx {\frac {2k_{\mathrm {B} }T\nu ^{2}}{c^{2}}}

Alternatively, Planck's law can be written as an expression $I(\nu ,T)=\pi B_{\nu }(T)$ for emitted power integrated over all solid angles. In this form, the Planck function and associated Rayleigh–Jeans limits are given by

I(\lambda ,T)={\frac {2\pi hc^{2}}{\lambda ^{5}}}~{\frac {1}{e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}-1}}\approx {\frac {2\pi ck_{\mathrm {B} }T}{\lambda ^{4}}}

or

I(\nu ,T)={\frac {2\pi h\nu ^{3}}{c^{2}}}{\frac {1}{e^{\frac {h\nu }{k_{\mathrm {B} }T}}-1}}\approx {\frac {2\pi k_{\mathrm {B} }T\nu ^{2}}{c^{2}}}

In other cases, Planck's law is written as ${\textstyle u(\nu ,T)={\frac {4\pi }{c}}B_{\nu }(T)}$ for energy per unit volume (energy density). In this form, the Planck function and associated Rayleigh–Jeans limits are given by

u(\lambda ,T)={\frac {8\pi hc}{\lambda ^{5}}}~{\frac {1}{e^{\frac {hc}{\lambda k_{\mathrm {B} }T}}-1}}\approx {\frac {8\pi k_{\mathrm {B} }T}{\lambda ^{4}}}

or

u(\nu ,T)={\frac {8\pi h\nu ^{3}}{c^{3}}}{\frac {1}{e^{\frac {h\nu }{k_{\mathrm {B} }T}}-1}}\approx {\frac {8\pi k_{\mathrm {B} }T\nu ^{2}}{c^{3}}}

References[]

^ ^a ^b Kutner, Mark L. (2003). Astronomy: A Physical Perspective. Cambridge University Press. p. 15. ISBN 0-521-52927-1.
^ Rybicki; Lightman (2004). Radiative Processes in Astrophysics. Wiley. pp. 20–28. ISBN 0-471-82759-2.

External links[]

Derivation at HyperPhysics

[auto-1] Kutner, Mark L. (2003). Astronomy: A Physical Perspective. Cambridge University Press. p. 15. ISBN 0-521-52927-1.

[2] Rybicki; Lightman (2004). Radiative Processes in Astrophysics. Wiley. pp. 20–28. ISBN 0-471-82759-2.

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