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{{Distinguish|Planck's relation}}
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{{See also |Black body radiation|Thermal radiation}}


[[File:Black body.svg|thumb|right|300px|Planck's law (colored curves) accurately described black body radiation, by proposing that [[electromagnetic radiation]] was emitted in [[quantum|quanta]]. It successfully resolved the [[ultraviolet catastrophe]] (black curve), a major problem of [[classical physics]], and is one of the pioneer results that gave birth to [[quantum mechanics]].]]
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In [[physics]], '''Planck's law''' describes the amount of electromagnetic energy with a certain wavelength radiated by a [[black body]] in [[thermal equilibrium]] (i.e. the [[spectral radiance]] of a black body). The law is named after [[Max Planck]], who originally proposed it in 1900. The law was the first to accurately describe black body radiation, and resolved the [[ultraviolet catastrophe]]. It is a pioneer result of [[modern physics]] and [[quantum mechanics|quantum theory]].
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In terms of frequency (<math>\nu</math>) or wavelength (''λ''), Planck's law is written:<ref name="Planck 1914 6 168">{{harvnb|Planck|1914|pp=6,&nbsp;168}}</ref><ref name="Chan8">{{harvnb|Chandrasekhar|1960|p=8}}</ref><ref name="Rybicki 1979 22">{{harvnb|Rybicki|Lightman|1979|p=22}}</ref>
'''MathML'''
:<math>B_\nu(T) = \frac{ 2 h \nu^3}{c^2} \frac{1}{e^\frac{h\nu}{k_\mathrm{B}T} - 1},\text{ or }\,B_\lambda(T) =\frac{2 hc^2}{\lambda^5}\frac{1}{ e^{\frac{hc}{\lambda k_\mathrm{B}T}} - 1}</math>
:<math forcemathmode="mathml">E=mc^2</math>


where ''B'' is the spectral radiance, ''T'' is the [[absolute temperature]] of the black body, ''k''<sub>B</sub> is the [[Boltzmann constant]], ''h'' is the [[Planck constant]], and ''c'' is the [[speed of light]]. However these are not the only ways to express the law; expressing it in terms of [[wavenumber]] rather than frequency or wavelength is also common, as are expression in terms of the number of photons emitted at a certain wavelength, rather than energy emitted. In the limit of low frequencies (i.e. long wavelengths), Planck's law becomes the [[Rayleigh–Jeans law]], while in the limit of high frequencies (i.e. small wavelengths) it tends to the [[Wien approximation]].
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:<math forcemathmode="png">E=mc^2</math>


[[Max Planck]] developed the law in 1900, originally with only empirically determined constants, and later showed that, expressed as an energy distribution, it is the unique stable distribution for radiation in [[thermodynamic equilibrium]].<ref name="Planck 1914 42">{{harvnb|Planck|1914|p=42}}</ref> As an energy distribution, it is one of a family of thermal equilibrium distributions which include the [[Bose–Einstein distribution]], the [[Fermi–Dirac distribution]] and the [[Maxwell–Boltzmann distribution]].
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== Introduction ==
<span style="color: red">Follow this [https://en.wikipedia.org/wiki/Special:Preferences#mw-prefsection-rendering link] to change your Math rendering settings.</span> You can also add a [https://en.wikipedia.org/wiki/Special:Preferences#mw-prefsection-rendering-skin Custom CSS] to force the MathML/SVG rendering or select different font families. See [https://www.mediawiki.org/wiki/Extension:Math#CSS_for_the_MathML_with_SVG_fallback_mode these examples].
Planck's law describes how much energy objects radiate, and more specifically how much energy of each frequency is radiated. It quantifies how objects at low temperatures radiate very little, hot objects glow a dull red and emit a perceptible amount of heat, and very hot objects (such as the sun) are dazzlingly bright yellow or blue-white.<!-- [This seems to be entirely redundant with the lead.] '''Planck's law''' expresses the quantity of [[thermal radiation]] emitted by a [[black body]], or ideal radiator, as a function of the absolute temperature ''T'' of the radiator and the frequency {{math|&nu;}} of the portion of spectrum being so expressed.  It is customarily expressed as
:<math>B_\nu(T)=\frac{2h\nu^3}{c^2}\frac1{e^{h\nu/kT}-1}</math>
where ''h'' is [[Planck's constant]], ''c'' is the [[speed of light]], and ''k'' is [[Boltzmann's constant]].--> The law gives the power radiated [[normal (geometry)|normally]] from a unit [[area]] of the radiator into unit [[solid angle]] within a [[frequency band]] of unit width centered on frequency {{math|&nu;}}. As such the [[spectral radiance]] {{math|''B''<sub>&nu;</sub>(''T'')}} has units of [[Watt|W]]·[[meter|m]]<sup>−2</sup>·[[steradian|sr]]<sup>−1</sup>·[[Hertz|Hz]]<sup>−1</sup> when stated in [[SI units]].<!-- [omitted for now] Since watts per Hertz is equivalent dimensionally to joules, and steradians are dimensionless, the units for Planck's law are dimensionally equivalent to joules per square meter. -->


This nominal meaning is however inaccurate because the radiation varies with both angle and frequency. It is made precise by shrinking unit area, unit solid angle, and unit bandwidth to their [[infinitesimal]] counterparts d''A'', dΩ, and {{math|d&nu;}}. The infinitesimal power radiated normally from a surface element d''A'' into solid angle dΩ within a band of width dν is then given by {{math|''B''<sub>&nu;</sub>(''T'')&nbsp;d''A''&nbsp;d&Omega;&nbsp;d&nu;}}.  The total radiated power over any region is obtained by [[integral|integration]] over that region with respect to those three quantities.
==Demos==


Much as the thermodynamics of ordinary gases composed of molecules can be understood using statistical mechanics, Planck's law can be derived by viewing the radiation as a gas of massless [[boson]]s (such as photons) in [[thermal equilibrium]]. If the temperature is changed, photons are created or annihilated in the right numbers and with the right energies to fill the cavity with a Planck distribution at the new temperature, and the pressure and energy density of a photon gas at equilibrium are entirely determined by the temperature. This is unlike the case for material gases, for which the pressure and energy density depend on the total number of particles and their properties, such as mass. In this way the Planck distribution arises as a limit of the [[Bose–Einstein distribution]], the energy distribution describing bosons in thermodynamic equilibrium.
Here are some [https://commons.wikimedia.org/w/index.php?title=Special:ListFiles/Frederic.wang demos]:


Radiation will obey Planck's law inside a [[resonator|cavity]] with opaque walls held at some fixed temperature, or near the surface of a [[black body]].  The radiation is [[isotropic]], [[homogeneous]], [[Polarization (waves)|unpolarized]], and [[Coherence (physics)|incoherent]], and the Planck distribution is the unique distribution for electromagnetic radiation in thermodynamic equilibrium.<ref name="Planck 1914">{{harvnb|Planck|1914}}</ref>


==Different forms==
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Planck's law can be encountered in several forms depending on the conventions and preferences of different scientific fields. The various forms of the law for spectral radiance are summarized in the table below. Forms on the left are most often encountered in [[experimental physics|experimental fields]], while those on the right are most often encountered in [[theoretical physics|theoretical fields]].
==Test pages ==
<center>
{|class="wikitable"
|+ Planck's law expressed in terms of different spectral variables<ref>{{harvnb|Caniou|1999|p=117}}</ref><ref>{{harvnb|Kramm|Mölders|2009}}</ref><ref name=SharkovConversions>{{harvnb|Sharkov|2003|p=210}}</ref>
|-
!colspan="2"|with ''h''
!colspan="2"|with '' ħ''
|-
!variable
!distribution
!variable
!distribution
|-
! [[Frequency]]<br><math>\nu</math>
| <math>B_\nu(T) =\frac{ 2 h\nu^{3}}{c^2} \frac{1}{e^{h\nu/(k_\mathrm{B}T)} - 1}</math>
! [[Angular frequency]]<br><math>\omega</math>
| <math>B_\omega(T) =\frac{ \hbar\omega^{3}}{4 \pi^3 c^2} \frac{1}{ e^{\hbar \omega/(k_\mathrm{B}T)} - 1 }</math>
|-
! [[Wavelength]]<br><math>\lambda</math>
| <math>B_\lambda(T) =\frac{2 hc^2}{\lambda^5} \frac{1}{e^{h c/(\lambda k_\mathrm{B}T)} - 1}</math>
! [[Angular wavelength]]<br><math>y</math>
| <math>B_y(T) =\frac{\hbar c^2}{4 \pi^3 y^5} \frac{1}{e^{\hbar c/(y k_\mathrm{B}T)}- 1}</math>
|-
! [[Wavenumber]]<br><math>\tilde{\nu}</math>
| <math>B_\tilde{\nu}(T) =2 hc^2\tilde{\nu}^3 \frac{1}{e^{hc\tilde{\nu}/(k_\mathrm{B}T)} - 1 }</math>
! [[Angular wavenumber]]<br><math>k</math>
| <math>B_k(T) = \frac{\hbar c^2 k^3}{4 \pi^3} \frac{1}{e^{\hbar c k/(k_\mathrm{B}T)} -1}</math>
|}
</center>


These distributions represent the spectral radiance of blackbodies&mdash;the power emitted from the emitting surface, per unit projected area of emitting surface, per unit [[solid angle]], per spectral unit (frequency, wavelength, wavenumber or their angular equivalents). Since the radiance is [[isotropy|isotropic]] (i.e. independent of direction), the power emitted at an angle to the [[normal (geometry)|normal]] is proportional to the projected area, and therefore to the cosine of that angle as per [[Lambert's cosine law]], and is [[polarization (waves)|unpolarized]].
To test the '''MathML''', '''PNG''', and '''source''' rendering modes, please go to one of the following test pages:
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===Correspondence between spectral variable forms===
*[[Inputtypes|Inputtypes (private Wikis only)]]
 
*[[Url2Image|Url2Image (private Wikis only)]]
Different spectral variables require different corresponding forms of expression of the law. In general, one may not convert between the various forms of Planck's law simply by substituting one variable for another, because this would not take into account that the different forms have different units.
==Bug reporting==
 
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Corresponding forms of expression are related because they express one and the same physical fact: For a particular physical spectral increment, a particular physical energy increment is radiated.
 
This is so whether it is expressed in terms of an increment of frequency, {{math|d''ν''}}, or, correspondingly, of wavelength, {{math|d''λ''}}. Introduction of a minus sign can indicate that an increment of frequency corresponds with decrement of wavelength. For the above corresponding forms of expression of the spectral radiance, one may use an obvious expansion of notation, temporarily for the present calculation only. Then, for a particular spectral increment, the particular physical energy increment may be written
 
:<math>B_\lambda ( \lambda,\ T) \ \mathrm d \lambda=-B_\nu(\nu ( \lambda),\ T) \ \mathrm d \nu\ ,</math>&nbsp;&nbsp;&nbsp;&nbsp; which leads to&nbsp;&nbsp;&nbsp;&nbsp;<math> B_\lambda(\lambda,\ T)\ =\ -\ \frac{\mathrm d \nu}{ \mathrm d \lambda}B_\nu(\nu (\lambda),\ T).</math>
 
Also, {{math|''ν''(''λ'') {{=}} ''c''/''λ''}}, so that {{math|d''ν''/d''λ'' {{=}} − ''c''/''λ''<sup>2</sup>}}.  Substitution gives the correspondence between the frequency and wavelength forms, with their different units.<ref name=SharkovConversions/><ref>{{harvnb|Goody|Yung|1989}}, p. 16.</ref>
 
It follows that the location of the peak of the distribution for Planck's law depends on the choice of spectral variable.
 
===Spectral energy density form===
Planck's law can also be written in terms of the spectral [[energy density]] (''u'') by multiplying ''B'' by 4π/''c'':<ref>{{harvnb|Fischer|2011}}</ref>
:<math>u_i(T) = \frac{4\pi}{c} B_i(T). </math>
 
These distributions have units of energy per volume per spectral unit.
 
== Derivation ==
{{See also|Gas in a box}}
Consider a cube of side ''L'' with conducting walls filled with electromagnetic radiation in thermal equilibrium at temperature T. If there is a small hole in one of the walls, the radiation emitted from the hole will be characteristic of a perfect [[black body]]. We will first calculate the spectral energy density within the cavity and then determine the spectral radiance of the emitted radiation.
 
At the walls of the cube, the parallel component of the electric field and the orthogonal component of the magnetic field must vanish. Analogous to the wave function of a [[particle in a box]], one finds that the fields are superpositions of periodic functions. The three wavelengths ''λ''<sub>1</sub>, ''λ''<sub>2</sub>, and ''λ''<sub>3</sub>, in the three directions orthogonal to the walls can be:
 
:<math>\lambda_i = \frac{2L}{n_{i}},</math>
 
where the ''n''<sub>i</sub> are integers. For each set of integers ''n''<sub>i</sub> there are two linear independent solutions (modes). According to quantum theory, the energy levels of a mode are given by:
 
:<math>E_{n_1,n_2,n_3}\left(r\right)=\left(r+\frac{1}{2}\right)\frac{hc}{2L}\sqrt{n_1^2 + n_2^2 + n_3^2}. \qquad \text{(1)}</math>
 
The quantum number ''r'' can be interpreted as the number of photons in the mode. The two modes for each set of ''n''<sub>i</sub> correspond to the two polarization states of the photon which has a spin of 1. Note that for {{nowrap|1=''r'' = 0}} the energy of the mode is not zero. This vacuum energy of the electromagnetic field is responsible for the [[Casimir effect]]. In the following we will calculate the internal energy of the box at [[absolute temperature]] ''T''.
 
According to [[statistical mechanics]], the probability distribution over the energy levels of a particular mode is given by:
 
:<math>P_r =\frac{\exp\left(-\beta E\left(r\right)\right)}{Z\left(\beta\right)}.</math>
 
Here
 
:<math>\beta\ \stackrel{\mathrm{def}}{=}\ 1/\left(kT\right).</math>
 
The denominator ''Z''(''β''), is the [[partition function (statistical mechanics)|partition function]] of a single mode and makes ''P''<sub>''r''</sub> properly normalized:
 
:<math>Z\left(\beta\right)=\sum_{r=0}^{\infty} e^{-\beta E\left(r\right)}=\frac{e^{-\beta\varepsilon/2}}{1-e^{-\beta\varepsilon}}.</math>
 
Here we have implicitly defined
 
:<math>\varepsilon\ \stackrel{\mathrm{def}}{=}\ \frac{hc}{2L}\sqrt{n_{1}^{2}+n_{2}^{2}+n_{3}^{2}},</math>
 
which is the energy of a single photon. As explained [[partition function (statistical mechanics)#Calculating the thermodynamic total energy|here]], the average energy in a mode can be expressed in terms of the partition function:
 
:<math>\left\langle E\right\rangle=-\frac{d\log\left(Z\right)}{d\beta}= \frac{\varepsilon}{2} + \frac{\varepsilon}{e^{\beta\varepsilon}-1}.</math>
 
This formula, apart from the first vacuum energy term, is a special case of the general formula for particles obeying [[Bose–Einstein statistics]]. Since there is no restriction on the total number of photons, the [[chemical potential]] is zero.
 
If we measure the energy relative to the ground state, the total energy in the box follows by summing <math>\scriptstyle{\left\langle E\right\rangle} - \frac{\varepsilon}{2}</math> over all allowed single photon states. This can be done exactly in the thermodynamic limit as ''L'' approaches infinity. In this limit, ''ε'' becomes continuous and we can then integrate <math>\scriptstyle{\left\langle E\right\rangle}- \frac{\varepsilon}{2}</math> over this parameter. To calculate the energy in the box in this way, we need to evaluate how many photon states there are in a given energy range. If we write the total number of single photon states with energies between ''ε'' and ''ε'' + ''dε'' as ''g''(''ε'')''dε'', where ''g''(''ε'') is the [[density of states]] (which we'll evaluate in a moment), then we can write:
 
:<math>U = \int_{0}^{\infty}\frac{\varepsilon}{e^{\beta\varepsilon}-1}g(\varepsilon)\,d\varepsilon. \qquad \mbox{(2)}</math>
 
To calculate the density of states we rewrite equation (1) as follows:
 
:<math>\varepsilon\ \stackrel{\mathrm{def}}{=}\ \frac{hc}{2L}n,</math>
 
where ''n'' is the norm of the vector {{nowrap|1='''n''' = (''n''<sub>1</sub>, ''n''<sub>2</sub>, ''n''<sub>3</sub>)}}:
 
:<math>n=\sqrt{n_{1}^{2}+n_{2}^{2}+n_{3}^{2}}.</math>
 
For every vector '''n''' with integer components larger than or equal to zero, there are two photon states. This means that the number of photon states in a certain region of ''n''-space is twice the volume of that region. An energy range of ''dε'' corresponds to shell of thickness ''dn'' = (2''L''/''hc'')''dε'' in ''n''-space. Because the components of '''n''' have to be positive, this shell spans an octant of a sphere. The number of photon states ''g''(''ε'')''dε'', in an energy range ''dε'', is thus given by:
 
:<math>g(\varepsilon)\,d\varepsilon=2\frac{1}{8}4\pi n^{2}\,dn=\frac{8\pi L^{3}}{h^{3}c^{3}}\varepsilon^{2}\,d\varepsilon.</math>
 
Inserting this in Eq. (2) gives:
 
:<math>U =L^3 \frac{8\pi}{h^3 c^3}\int_0^\infty \frac{\varepsilon^3}{e^{\beta\varepsilon}-1}\,d\varepsilon. \qquad \text{(3)}</math>
 
From this equation one easily derives the spectral energy density as a function of frequency <math>u_\nu(T)</math> and as a function of wavelength ''u''<sub>''λ''</sub>(''T''):
 
:<math>\frac{U}{L^3} = \int_0^\infty u_\nu(T)\, d\nu,</math>
 
where:
 
:<math>u_\nu(T) = {8\pi h\nu^3\over c^3}{1\over e^{h\nu/k_\mathrm{B}T} - 1}.</math>
 
And:
 
:<math>\frac{U}{L^3} = \int_0^\infty u_\lambda(T)\, d\lambda,</math>
 
where
 
:<math>u_\lambda(T) = {8\pi h c\over \lambda^5}{1\over e^{h c/\lambda k_\mathrm{B}T} - 1}.</math>
 
This is also a spectral energy density function with units of energy per unit wavelength per unit volume. Integrals of this type for Bose and Fermi gases can be expressed in terms of [[polylogarithm]]s. In this case, however, it is possible to calculate the integral in closed form using only elementary functions. Substituting
 
:<math>\varepsilon = k_\mathrm{B}Tx,</math>
 
in Eq. (3), makes the integration variable dimensionless giving:
 
:<math>u(T) =\frac{8\pi (k_\mathrm{B}T)^{4}}{(hc)^{3}} J,</math>
 
where ''J'' is a [[Bose–Einstein integral]] given by:
 
:<math>J=\int_{0}^{\infty}\frac{x^{3}}{e^x - 1}\,dx = \frac{\pi^{4}}{15}.</math>
 
The total electromagnetic energy inside the box is thus given by:
 
:<math>{U\over V} = \frac{8\pi^5(k_\mathrm{B}T)^4}{15 (hc)^3},</math>
 
where ''V'' = ''L''<sup>3</sup> is the volume of the box.
 
This is '''not''' the [[Stefan–Boltzmann law]] (which provides the total energy ''radiated'' by a black body per unit surface area per unit time), but it can be written more compactly using the [[Stefan–Boltzmann constant]] ''σ'', giving
 
:<math>{U\over V} = \frac{4 \sigma T^4}{c}.</math>
 
The constant 4''σ''/''c'' is sometimes called the radiation constant.
 
Since the radiation is the same in all directions, and propagates at the speed of light (''c''), the spectral radiance of radiation exiting the small hole is
 
:<math>B_\nu(T) = \frac{u_\nu(T)\,c}{4\pi},</math>
 
which yields
 
:<math>B_\nu(T) = \frac{2 h\nu^3 }{c^2}~\frac{1}{e^{h\nu/k_\mathrm{B}T}-1}.</math>
 
It can be converted to an expression for ''B''<sub>''λ''</sub>''(T'') in wavelength units by substituting <math>\nu</math> by ''c/λ'' and evaluating
:<math>B_\lambda(T) = B_\nu(T)\left|\frac{d\nu}{d\lambda}\right|.</math>
 
Note that dimensional analysis shows that the unit of steradians, shown in the denominator of left hand side of the equation above, is generated in and carried through the derivation but does not appear in any of the dimensions for any element on the left-hand-side of the equation.
 
This derivation is based on {{harvnb|Brehm|Mullin|1989}}.
 
==Physics==
 
===Outline===
 
Planck's law describes the unique and characteristic spectral distribution for electromagnetic radiation in thermodynamic equilibrium, when there is no net flow of matter or energy.<ref name="Planck 1914 42"/> Its physics is most easily understood by considering the radiation in a cavity with rigid opaque walls. Motion of the walls can affect the radiation. If the walls are not opaque, then the thermodynamic equilibrium is not isolated. It is of interest to explain how the thermodynamic equilibrium is attained. There are two main cases: (a) when the approach to thermodynamic equilibrium is in the presence of matter, when the walls of the cavity are imperfectly reflective for every wavelength or when the walls are perfectly reflective while the cavity contains a small black body (this was the main case considered by Planck); or (b) when the approach to equilibrium is in the absence of matter, when the walls are perfectly reflective for all wavelengths and the cavity contains no matter. For matter not enclosed in such a cavity, thermal radiation can be approximately explained by appropriate use of Planck's law.
 
Classical physics provides an account of some aspects of the Planck distribution, such as the [[Stefan–Boltzmann law]], and the [[Wien displacement law]]. Other aspects of the Planck distribution cannot be accounted for in classical physics, and require quantum theory for their understanding. For the case of the presence of matter, quantum mechanics provides a good account, as found below in the section headed [[Planck's law#Physics#Einstein coefficients|Einstein coefficients]]. This was the case considered by Einstein, and is nowadays used for quantum optics.<ref>{{harvnb|Loudon|2000}}</ref><ref>{{harvnb|Mandel|Wolf|1995}}</ref> For the case of the absence of matter, quantum field theory is called upon, because quantum mechanics alone does not provide a sufficient account.
 
Quantum theoretical explanation of Planck's law views the radiation as a gas of massless, uncharged, bosonic particles, namely photons, in thermodynamic equilibrium.  Photons are viewed as the carriers of the electromagnetic interaction between electrically charged elementary particles. Photon numbers are not conserved.  Photons are created or annihilated in the right numbers and with the right energies to fill the cavity with the Planck distribution.  The pressure and energy density of a photon gas at equilibrium are entirely determined by the temperature. This is unlike the case for material gases, for which the pressure and energy density depend on the molecular masses and other characteristics of the constituent particles. For a material gas at given temperature, the pressure and energy density can vary independently for different gases, because different molecules can carry different excitation energies.
 
Planck's law arises as a limit of the [[Bose–Einstein distribution]], the energy distribution describing non-interactive [[bosons]] in thermodynamic equilibrium. In the case of massless bosons such as [[photons]] and [[gluons]], the [[chemical potential]] is zero and the Bose-Einstein distribution reduces to the Planck distribution.  There is another fundamental equilibrium energy distribution: the [[Fermi–Dirac distribution]], which describes [[fermions]], such as electrons, in thermal equilibrium. The two distributions differ because multiple bosons can occupy the same quantum state, while multiple fermions cannot. At low densities, the number of available quantum states per particle is large, and this difference becomes irrelevant. In the low density limit, the Bose-Einstein and the Fermi-Dirac distribution each reduce to the [[Maxwell–Boltzmann distribution]].
 
=== Kirchhoff's law ===
{{main|Kirchhoff's law of thermal radiation}}
If there is a material body in [[thermal equilibrium]] with the radiation field, then the radiation power falling upon a small area element of that body must be equal to the amount of radiation power leaving that element. There are two ways that radiation may leave such an area element – reflection or scattering and emission. This assumes that the material body is large enough to be opaque – there is no radiation leaving the element that has been transmitted through the body. At a particular frequency, the power directed into the area element at equilibrium will be equal to the equilibrium distribution <math>B_\nu</math> (without necessarily specifying what that distribution is). Defining <math>\alpha</math> as the fraction of incident radiation absorbed at the surface, the rate at which this energy is absorbed will be <math>\alpha B_\nu</math>. By conservation of energy, the rest must be reflected or scattered, which will be proportional to <math>(1-\alpha) B_\nu</math>. The area element will also emit its own thermal radiation which may be expressed as a proportion of the equilibrium radiation: <math>\varepsilon B_\nu</math>, where <math>\varepsilon</math> is the [[emissivity]] of the surface. Since, at equilibrium, the rate of energy arriving must equal the rate leaving, it follows that:
 
:<math>B_\nu = (1-\alpha)B_\nu+\varepsilon B_\nu \, </math>
 
or, equivalently <math>\alpha=\varepsilon</math>, which is just [[Kirchhoff's law of thermal radiation|Kirchhoff's law]] applied to that surface element.{{Citation needed|date=November 2011}} It is generally true that the emissivity and absorptivity are properties of the material only, so that this equivalence will hold even when the radiation field is not thermal radiation. Kirchhoff's law also implies that the equilibrium distribution is unique, and Planck's contribution was to determine the expression of that equilibrium distribution.
 
=== Black body ===
{{main|Black body}}
A black body completely absorbs all of the electromagnetic radiation falling upon it (hence the term "black"). This means that <math>\alpha=1</math>, and by Kirchhoff's law, the emissivity will be unity as well, so that the thermal radiation from a black body is always equal to the full amount specified by Planck's law. In addition, it follows that no other body can emit thermal radiation that exceeds that of a black body, since if it were in equilibrium with a radiation field, it would be emitting more energy than was incident upon it.
 
Though perfectly black materials do not exist, in practice a black surface can be accurately approximated.<ref name="Planck 1914 42"/> As to its material interior, a body is completely black to a certain wavelength if it is completely opaque to that wavelength; that means that it absorbs all of the wavelength that penetrates the interface to enter the body; this is not too difficult to achieve in practice. On the other hand, a perfectly black interface is not found in nature. The best practical way to make an effectively black interface is to simulate an 'interface' by use of a small hole in the wall of a large cavity in a completely opaque body, with a controlled temperature. Radiation entering the hole has almost no possibility of escaping the cavity without being absorbed by multiple impacts with its walls.<ref>{{harvnb|Siegel|Howell|2002|p=25}}</ref>
 
=== Lambert's cosine law ===
{{main|Lambert's cosine law}}
 
As explained by Planck,<ref>{{harvnb|Planck|1914|pp=9–11}}</ref> a radiating body has an interior consisting of matter, and an interface with its contiguous neighbouring material medium, which is usually the medium from within which the radiation from the surface of the body is observed. The interface is not composed of physical matter but is a theoretical conception, a mathematical two-dimensional surface, a joint property of the two contiguous media, strictly speaking belonging to neither separately. Such an interface can neither absorb nor emit, because it is not composed of physical matter; but it is the site of reflection and transmission of radiation, because it is a surface of discontinuity of optical properties. The reflection and transmission of radiation at the interface obey the [[Helmholtz reciprocity|Stokes–Helmholtz reciprocity principle]].
 
At any point in the interior of a black body located inside a cavity in thermodynamic equilibrium at temperature {{math|''T''}} the radiation is homogeneous, isotropic and unpolarized. A black body absorbs all and reflects none of the electromagnetic radiation incident upon it. According to the Helmholtz reciprocity principle, radiation from the interior of a black body is not reflected at its surface, but is fully transmitted to its exterior. Because of the isotropy of the radiation in the body's interior, the [[spectral radiance]] of radiation transmitted from its interior to its exterior through its surface is independent of direction.<ref>{{harvnb|Planck|1914|page=35}}</ref>
 
This is expressed by saying that radiation from the surface of a black body in thermodynamic equilibrium obeys Lambert's cosine law.<ref>{{harvnb|Landsberg|1961|pages=273–274}}</ref><ref>{{harvnb|Born|Wolf|1999|pp=194–199}}</ref> This means that the spectral flux {{math|dΦ(d''A'', ''θ'', dΩ, d''ν'')}} from a given infinitesimal element of area {{math|d''A''}} of the actual emitting surface of the black body, detected from a given direction that makes an angle {{math|''θ''}} with the normal to the actual emitting surface at {{math|d''A''}}, into an element of solid angle of detection {{math|dΩ}} centred on the direction indicated by {{math|''θ''}}, in an element of frequency bandwidth {{math|d''ν''}}, can be represented as<ref>{{harvnb|Born|Wolf|1999|page=195}}</ref>
 
:<math>\frac{\mathrm{d} \Phi(\mathrm{d}A,\theta,\mathrm{d}\Omega,\mathrm{d}\nu)}{\mathrm{d}\Omega} = L^0(\mathrm{d}A,\mathrm{d}\nu)\,\mathrm{d}A\,\mathrm{d}\nu\,\cos \theta</math>
 
where {{math|''L''<sup>0</sup>(d''A'', d''ν'')}} denotes the flux, per unit area per unit frequency per unit solid angle, that area {{math|d''A''}} would show if it were measured in its normal direction {{math|''θ'' {{=}} 0}}.
 
The factor {{math|cos ''θ''}} is present because the area to which the spectral radiance refers directly is the projection, of the actual emitting surface area, onto a plane perpendicular to the direction indicated by {{math|''θ''}} . This is the reason for the name ''cosine law''.
 
Taking into account the independence of direction of the spectral radiance of radiation from the surface of a black body in thermodynamic equilibrium, one has {{math|''L''<sup>0</sup>(d''A'', d''ν'') {{=}} ''B''<sub>''ν''</sub> (''T'')}} and so
 
:<math>\frac{\mathrm{d} \Phi(\mathrm{d}A,\theta,\mathrm{d}\Omega,\mathrm{d}\nu)}{\mathrm{d}{\Omega}}= B_\nu (T)\,\mathrm{d}A\,\mathrm{d}\nu\,\cos\theta.</math>
 
Thus Lambert's cosine law expresses the independence of direction of the spectral radiance {{math|''B''<sub>''ν''</sub> (''T'')}} of the surface of a black body in thermodynamic equilibrium.
 
=== Stefan–Boltzmann law ===
{{main|Stefan–Boltzmann law}}
 
The total power emitted per unit area at the surface of a black body (''P'') may be found by integrating the black body spectral flux found from Lambert's law over all frequencies, and over the solid angles corresponding to a hemisphere (''h'') above the surface.
 
:<math>P=\int_0^\infty d\nu \int_h d\Omega\,B_\nu \cos(\theta)</math>
 
The infinitesimal solid angle can be expressed in [[spherical polar coordinates]]:
 
:<math>d\Omega=\sin(\theta)\,d\theta\,d\phi.</math>
 
So that:
 
:<math>P=\int_0^\infty d\nu \int_0^{\pi/2} d\theta \int_0^{2\pi}d\phi \, B_\nu(T) \cos(\theta)\sin(\theta)=\sigma\,T^4</math>
 
where
 
:<math>\sigma=\frac{2k^4\pi^5}{15c^2h^3}\approx 5.670 400 \times 10^{-8}\, \mathrm{J\, s^{-1}m^{-2}K^{-4}}</math>
 
is known as the [[Stefan–Boltzmann constant]].<ref name="Rybicki 1979 19">{{harvnb|Rybicki|Lightman|1979|p=19}}</ref>
 
=== Radiative transfer ===
{{main|Radiative transfer}}
 
The equation of radiative transfer describes the way in which radiation is affected as it travels through a material medium. For the special case in which the material medium is in [[thermodynamic equilibrium]] in the neighborhood of a point in the medium, Planck's law is of special importance.
 
For simplicity, we can consider the linear steady state, without [[scattering]]. The equation of radiative transfer states that for a beam of light going through a small distance ''ds'', energy is conserved: The change in the (spectral) [[radiance]] of that beam (<math>I_\nu</math>) is equal to the amount removed by the material medium plus the amount gained from the material medium. If the radiation field is in equilibrium with the material medium, these two contributions will be equal. The material medium will have a certain [[emission coefficient]] and [[absorption coefficient]].
 
The absorption coefficient <math>\alpha</math> is the fractional change in the intensity of the light beam as it travels the distance ''ds'', and has units of 1/length. It is composed of two parts, the decrease due to absorption and the increase due to [[stimulated emission]]. Stimulated emission is emission by the material body which is caused by and is proportional to the incoming radiation. It is included in the absorption term because, like absorption, it is proportional to the intensity of the incoming radiation. Since the amount of absorption will generally vary linearly as the density <math>\rho</math> of the material, we may define a "mass absorption coefficient" <math>\kappa_\nu=\alpha/\rho</math> which is a property of the material itself. The change in intensity of a light beam due to absorption as it traverses a small distance ''ds'' will then be <math>dI_\nu=-\kappa_\nu\,\rho\,I_\nu\,ds</math><ref name="Chan8"/>
 
The "mass emission coefficient" <math>j_\nu</math> is equal to the radiance per unit volume of a small volume element divided by its mass (since, as for the mass absorption coefficient, the emission is proportional to the emitting mass) and has units of power/solid angle/frequency/density. Like the mass absorption coefficient, it too is a property of the material itself. The change in a light beam as it traverses a small distance ''ds'' will then be <math>dI_\nu=j_\nu\,\rho\,ds</math><ref name="Chan7">{{harvnb|Chandrasekhar|1960|p=7}}</ref>
 
The equation of radiative transfer will then be the sum of these two contributions:<ref name="Chan9">{{harvnb|Chandrasekhar|1960|p=9}}</ref>
 
:<math>\frac{dI_\nu}{ds}=j_\nu\rho-k_\nu\rho I_\nu.</math>
 
If the radiation field is in equilibrium with the material medium, then the radiation will be homogeneous (independent of position) so that <math>dI_\nu=0</math> and:
 
:<math>k_\nu B_\nu = j_\nu\,</math>
 
which is another statement of Kirchhoff's law, relating two material properties of the medium, and which yields the radiative transfer equation at a point around which the medium is in thermodynamic equilibrium:
 
:<math>\frac{dI_\nu}{ds}=k_\nu\rho(B_\nu-I_\nu).</math>
 
=== Einstein coefficients ===
{{main|Atomic spectral line}}
 
The principle of [[detailed balance]] states that, at thermodynamic equilibrium, each elementary process is equilibrated by its reverse process.
 
In 1916, [[Albert Einstein]] applied this principle on an atomic level to the case of an atom radiating and absorbing radiation due to transitions between two particular energy levels,<ref name="Einstein 1916"/> giving a deeper insight into the equation of radiative transfer and Kirchhoff's law for this type of radiation. If level 1 is the lower energy level with energy <math>E_1</math>, and level 2 is the upper energy level with energy <math>E_2</math>, then the frequency <math>\nu</math> of the radiation radiated or absorbed will be determined by Bohr's frequency condition: <math>E_2-E_1=h\nu</math>.<ref name="Bohr 1913"/><ref name="Jammer 1989 113 115"/>
 
If <math>n_1</math> and <math>n_2</math> are the number densities of the atom in states 1 and 2 respectively, then the rate of change of these densities in time will be due to three processes:
 
:{|cellpadding="12"
|-
| <math>\left(\frac{dn_1}{dt}\right)_\mathrm{spon}=A_{21} n_2</math>
| Spontaneous emission
|-
| <math>\left(\frac{dn_1}{dt}\right)_\mathrm{stim}=B_{21} n_2 I_\nu(T)</math>
| Stimulated emission
|-
| <math>\left(\frac{dn_2}{dt}\right)_\mathrm{abs}=B_{12} n_1 I_\nu(T)</math>
| Photo-absorption
|}
 
where <math>I_\nu(T)</math> is the spectral radiance of the radiation field. The three parameters <math>A_{21}</math>, <math>B_{21}</math> and <math>B_{12}</math>, known as the Einstein coefficients, are associated with the photon frequency <math>(\nu)</math> produced by the transition between two energy levels (states). As a result, each line in a spectra has it own set of associated coefficients. When the atoms and the radiation field are in equilibrium, the radiance will be given by Planck's law and, by the principle of detailed balance, the sum of these rates must be zero:
 
:<math>0=A_{21}n_2+B_{21}n_2 B_\nu(T)-B_{12}n_1 B_\nu(T)\,</math>
 
Since the atoms are also in equilibrium, the populations of the two levels are related by the [[Boltzmann distribution]]:
 
:<math>\frac{n_2}{n_1}=\frac{g_2}{g_1} e^{-h\nu/k_B T}</math>
 
where <math>g_1</math> and <math>g_2</math> are the multiplicities of the respective energy levels. Combining the above two equations with the requirement that they be valid at any temperature yields two relationships between the Einstein coefficients:
 
:<math>\frac{A_{21}}{B_{21}}=\frac{2h\nu^3}{c^2}</math>
 
:<math>\frac{B_{21}}{B_{12}}=\frac{g_1}{g_2}</math>
 
so that knowledge of one coefficient will yield the other two. For the case of isotropic absorption and emission, the emission coefficient (<math>j_\nu</math>) and absorption coefficient (<math>\kappa_\nu\,</math>) defined in the radiative transfer section above, can be expressed in terms of the Einstein coefficients. The relationships between the Einstein coefficients will yield the expression of Kirchhoff's law expressed in the [[Planck's law#Radiative transfer|''Radiative transfer'']] section above, namely that
 
:<math>j_\nu=\kappa_\nu B_\nu.\,</math>
 
These coefficients apply to both atoms and molecules.
 
==Properties==
 
===Peaks===
The distributions <math>B_\nu, B_\omega, B_\tilde{\nu}</math> and <math>B_k</math> peak at<ref name=KK-Peak>{{harvnb|Kittel|Kroemer|1980|p=98}}</ref>
 
:<math>E = \left[ 3 + W \left(\frac{-3}{e^3} \right) \right] k_\mathrm{B}T \approx 2.821\ k_\mathrm{B}T,</math>
 
where ''W'' is the [[Lambert W function]].
 
The distributions <math>B_\lambda</math> and <math>B_y</math> however, peak at a different energy<ref name=KK-Peak/>
 
:<math>E = \left[ 5 + W \left(\frac{-5}{e^5} \right) \right] k_\mathrm{B}T \approx 4.965\ k_\mathrm{B}T,</math>
 
The reason for this is that, as mentioned above, one cannot go from (for example) <math>B_\nu</math> to <math>B_\lambda</math> simply by substituting <math>\nu</math> by <math>\lambda</math>. In addition, one must also multiply the result of the substitution by <math>\left | \frac{d\nu}{d\lambda} \right| = c/\lambda^2</math>. This <math>1/\lambda^2</math> factor shifts the peak of the distribution to higher energies.
 
===Approximations===
<small>[[Image:RWP-comparison.svg|thumb|right|310px|Log-log plots of radiance vs. frequency for Planck's law (green), compared with the [[Rayleigh–Jeans law]] (red) and the [[Wien approximation]] (blue) for a black body at 8 mK [[temperature]].]]</small>
 
In the limit of low frequencies (i.e. long wavelengths), Planck's law becomes the [[Rayleigh–Jeans law]]<ref name="Jeans 1905a">{{harvnb|Jeans|1905a|page=98}}</ref><ref name="Rayleigh 1905">{{harvnb|Rayleigh|1905}}</ref><ref name="Rybicki 1979 23">{{harvnb|Rybicki|Lightman|1979|p=23}}</ref>
 
:<math>B_\nu(T) \approx \frac{2 \nu^2 }{c^2}\,k_\mathrm{B} T</math>&nbsp;&nbsp;&nbsp;&nbsp; or &nbsp;&nbsp;&nbsp;&nbsp;<math>\qquad B_\lambda(T) \approx \frac{2c}{\lambda^4}\,k_\mathrm{B} T.</math>
 
The radiance increases as the square of the frequency, illustrating the [[ultraviolet catastrophe]]. In the limit of high frequencies (i.e. small wavelengths) Planck's law tends to the [[Wien approximation]]:<ref name="Rybicki 1979 23"/><ref name="Wien 1896 667">{{harvnb|Wien|1896|page=667}}</ref><ref>{{harvnb|Planck|1906|page=158}}</ref>
 
:<math>B_\nu(T) \approx \frac{2 h \nu^3}{c^2}\,e^{-\frac{h \nu}{k_\mathrm{B}T}}</math>&nbsp;&nbsp;&nbsp;&nbsp; or &nbsp;&nbsp;&nbsp;&nbsp;<math>B_\lambda(T) \approx \frac{2 h c^2}{\lambda^5}\,e^{-\frac{hc}{\lambda k_\mathrm{B} T}}.</math>
 
Both approximations were known to Planck before he developed his law. He was led by these two approximations to develop a law which incorporated both limits, which ultimately became Planck's law.
 
===Percentiles===
[[File:EffectiveTemperature 300dpi e.png|thumb|left|The Sun is an excellent approximation of a black body. Its [[effective temperature]] is ~{{val|5777|u=K}}.]]
[[Wien's displacement law]] in its stronger form states that the shape of Planck's law is independent of temperature. It is therefore possible to list the percentile points of the total radiation as well as the peaks for wavelength and frequency, in a form which gives the wavelength ''λ'' when divided by temperature ''T''.<ref>{{harvnb|Lowen|Blanch|1940}}</ref> The second row of the following table lists the corresponding values of ''λT'', that is, those values of ''x'' for which the wavelength ''λ'' is ''x''/''T'' [[micrometer (unit)|micrometers]] at the radiance percentile point given by the corresponding entry in the first row.
 
<center>
{| class=wikitable style="text-align:center;"
|-
! Percentile
| 0.01% || 0.1% || 1% || 10% || 20% || '''25.0%''' || 30% || 40% || '''41.8%''' || 50% || 60% || '''64.6%''' || 70% || 80% || 90% || 99% || 99.9% || 99.99%
|-
! ''λT'' (μm·K)
| 910 || 1110 || 1448 || 2195 || 2676 || '''2898''' || 3119 || 3582 || '''3670''' || 4107 || 4745 || '''5099''' || 5590 || 6864 || 9376 || 22884 || 51613 || 113374
|}
</center>
 
That is, 0.01% of the radiation is at a wavelength below 910/''T'' µm, 20% below 2676/''T'' µm, etc. The wavelength and frequency peaks are in bold and occur at 25.0% and 64.6% respectively. The 41.8% point is the wavelength-frequency-neutral peak. These are the points at which the respective Planck-law functions <math>1/\lambda^5</math>, <math>\nu^3</math>, and <math>\nu^2/\lambda^2</math> divided by {{nowrap|exp(''h&nu;''/''k''<sub>B</sub>''T'') − 1}} attain their maxima. Also note the much smaller gap in ratio of wavelengths between 0.1% and 0.01% (1110 is 22% more than 910) than between 99.9% and 99.99% (113374 is 120% more than 51613), reflecting the exponential decay of energy at short wavelengths (left end) and polynomial decay at long.
 
Which peak to use depends on the application. The conventional choice is the wavelength peak at 25.0% given by [[Wien's displacement law]] in its weak form. For some purposes the median or 50% point dividing the total radiation into two halves may be more suitable. The latter is closer to the frequency peak than to the wavelength peak because the radiance drops exponentially at short wavelengths and only polynomially at long. The neutral peak occurs at a shorter wavelength than the median for the same reason.
 
For the Sun, ''T'' is 5778 K, allowing the percentile points of the Sun's radiation, in nanometers, to be tabulated as follows when modeled as a black body radiator, to which the Sun is a fair approximation. For comparison a planet modeled as a black body radiating at a nominal 288 K (15 °C) as a representative value of the Earth's highly variable temperature has wavelengths more than twenty times that of the Sun, tabulated in the third row in micrometers (thousands of nanometers).
 
<center>
{| class=wikitable style="text-align:center;"
|-
! Percentile
| 0.01% || 0.1% || 1% || 10%|| 20%|| '''25.0%''' || 30%|| 40%|| '''41.8%''' || 50%|| 60%|| '''64.6%''' || 70%|| 80%|| 90% || 99% || 99.9% || 99.99%
|-
! Sun ''λ'' (nm)
| 157 || 192 || 251 || 380 || 463 || '''502'''|| 540 || 620 || '''635''' || 711 || 821 ||'''882''' || 967 || 1188 || 1623 || 3961 || 8933 || 19620
|-
! 288 K planet ''λ'' (µm)
| 3.16 || 3.85 || 5.03 || 7.62 || 9.29 || '''10.1''' || 10.8 || 12.4 || '''12.7''' || 14.3 || 16.5 || '''17.7''' || 19.4 || 23.8 || 32.6 || 79.5 || 179 || 394
|}
</center>
 
That is, only 1% of the Sun's radiation is at wavelengths shorter than 251&nbsp;nm, and only 1% at longer than 3961&nbsp;nm. Expressed in micrometers this puts 98% of the Sun's radiation in the range from 0.251 to 3.961&nbsp;µm. The corresponding 98% of energy radiated from a 288 K planet is from 5.03 to 79.5&nbsp;µm, well above the range of solar radiation (or below if expressed in terms of frequencies <math>\nu=c/\lambda</math> instead of wavelengths <math>\lambda</math>).
 
A consequence of this more-than-order-of-magnitude difference in wavelength between solar and planetary radiation is that filters designed to pass one and block the other are easy to construct. For example windows fabricated of ordinary glass or transparent plastic pass at least 80% of the incoming 5778 K solar radiation, which is below 1.2&nbsp;µm in wavelength, while blocking over 99% of the outgoing 288 K thermal radiation from 5&nbsp;µm upwards, wavelengths at which most kinds of glass and plastic of construction-grade thickness are effectively opaque.
 
The Sun's radiation is that arriving at the top of the atmosphere (TOA). As can be read from the table, radiation below 400&nbsp;nm, or [[ultraviolet]], is about 12%, while that above 700&nbsp;nm, or [[infrared]], starts at about the 49% point and so accounts for 51% of the total. Hence only 37% of the TOA insolation is visible to the human eye. The atmosphere shifts these percentages substantially in favor of visible light as it absorbs most of the ultraviolet and significant amounts of infrared.
 
== History ==
 
===Forerunners===
 
====Balfour Stewart====
 
In 1858, [[Balfour Stewart]] described his experiments on the thermal radiative emissive and absorptive powers of polished plates of various substances, compared with the powers of lamp-black surfaces, at the same temperature.<ref name="Stewart 1858">{{harvnb|Stewart|1858}}</ref> Stewart chose lamp-black surfaces as his reference because of various previous experimental findings, especially those of [[Pierre Prevost]] and of [[John Leslie (physicist)|John Leslie]]. He wrote "Lamp-black, which absorbs all the rays that fall upon it, and therefore possesses the greatest possible absorbing power, will possess also the greatest possible radiating power."
 
Stewart measured radiated power with a thermo-pile and sensitive galvanometer read with a microscope. He was concerned with selective thermal radiation, which he investigated with plates of substances that radiated and absorbed selectively for different qualities of radiation rather than maximally for all qualities of radiation. He discussed the experiments in terms of rays which could be reflected and refracted, and which obeyed the [[Helmholtz reciprocity|Helmholtz reciprocity principle]] (though he did not use an eponym for it). He did not in this paper mention that the qualities of the rays might be described by their wavelengths, nor did he use spectrally resolving apparatus such as prisms or diffraction gratings. His work was quantitative within these constraints. He made his measurements in a room temperature environment, and quickly so as to catch his bodies in a condition near the thermal equilibrium in which they had been prepared by heating to equilibrium with boiling water. His measurements confirmed that substances that emit and absorb selectively respect the principle of selective equality of emission and absorption at thermal equilibrium.
 
Stewart offered a theoretical proof that this should be the case separately for every selected quality of thermal radiation, but his mathematics was not rigorously valid. According to historian D.M Siegel: "He was not a practitioner of the more sophisticated techniques of nineteenth-century mathematical physics; he did not even make use of the functional notation in dealing with spectral distributions."<ref name="Siegel">{{harvnb|Siegel|1976}}</ref> He made no mention of thermodynamics in this paper, though he did refer to conservation of ''vis viva''. He proposed that his measurements implied that radiation was both absorbed and emitted by particles of matter throughout depths of the media in which it propagated. He applied the Helmholtz reciprocity principle to account for the material interface processes as distinct from the processes in the interior material. He concluded that his experiments showed that, in the interior of an enclosure in thermal equilibrium, the radiant heat, reflected and emitted combined, leaving any part of the surface, regardless of its substance, was the same as would have left that same portion of the surface if it had been composed of lamp-black. He did not mention the possibility of ideally perfectly reflective walls; in particular he noted that highly polished real physical metals absorb very slightly.
 
====Gustav Kirchhoff====
 
In 1859, not knowing of Stewart's work, [[Gustav Robert Kirchhoff]] reported the coincidence of the wavelengths of spectrally resolved lines of absorption and of emission of visible light. Importantly for thermal physics, he also observed that bright lines or dark lines were apparent depending on the temperature difference between emitter and absorber.<ref>{{harvnb|Kirchhoff|1860a}}</ref>
 
Kirchhoff then went on to consider bodies that emit and absorb heat radiation, in an opaque enclosure or cavity, in equilibrium at temperature {{math|''T''}}.
 
Here is used a notation different from Kirchhoff's. Here, the emitting power {{math|''E''(''T'', ''i'')}} denotes a dimensioned quantity, the total radiation emitted by a body labeled by index {{math|''i''}} at temperature {{math|''T''}}. The total absorption ratio {{math|''a''(''T'', ''i'')}} of that body is dimensionless, the ratio of absorbed to incident radiation in the cavity at temperature {{math|''T''}} . (In contrast with Balfour Stewart's, Kirchhoff's definition of his absorption ratio did not refer in particular to a lamp-black surface as the source of the incident radiation.) Thus the ratio {{math|''E''(''T'', ''i'') / ''a''(''T'', ''i'')}} of emitting power to absorption ratio is a dimensioned quantity, with the dimensions of emitting power, because {{math|''a''(''T'', ''i'')}} is dimensionless. Also here the wavelength-specific emitting power of the body at temperature {{math|''T''}} is denoted by {{math|''E''(''λ'', ''T'', ''i'')}} and the wavelength-specific absorption ratio by {{math|''a''(''λ'', ''T'', ''i'')}} . Again, the ratio {{math|''E''(''λ'', ''T'', ''i'') / ''a''(''λ'', ''T'', ''i'')}} of emitting power to absorption ratio is a dimensioned quantity, with the dimensions of emitting power.
 
In a second report made in 1859, Kirchhoff announced a new general principle or law for which he offered a theoretical and mathematical proof, though he did not offer quantitative measurements of radiation powers.<ref>{{harvnb|Kirchhoff|1860b}}</ref> His theoretical proof was and still is considered by some writers to be invalid.<ref name="Siegel"/><ref name="Schirrmacher 2001">{{harvnb|Schirrmacher|2001}}</ref> His principle, however, has endured: it was that for heat rays of the same wavelength, in equilibrium at a given temperature, the wavelength-specific ratio of emitting power to absorption ratio has one and the same common value for all bodies that emit and absorb at that wavelength. In symbols, the law stated that the wavelength-specific ratio {{math|''E''(''λ'', ''T'', ''i'') / ''a''(''λ'', ''T'', ''i'')}} has one and the same value for all bodies, that is for all values of index {{math|''i''}} . In this report there was no mention of black bodies.
 
In 1860, still not knowing of Stewart's measurements for selected qualities of radiation, Kirchhoff pointed out that it was long established experimentally that for total heat radiation, of unselected quality, emitted and absorbed by a body in equilibrium, the dimensioned total radiation ratio {{math|''E''(''T'', ''i'') / ''a''(''T'', ''i'')}}, has one and the same value common to all bodies, that is, for every value of the material index {{math|''i''}}.<ref name="Kirchhoff 1860c">{{harvnb|Kirchhoff|1860c}}</ref> Again without measurements of radiative powers or other new experimental data, Kirchhoff then offered a fresh theoretical proof of his new principle of the universality of the value of the wavelength-specific ratio {{math|''E''(''λ'', ''T'', ''i'') / ''a''(''λ'', ''T'', ''i'')}} at thermal equilibrium. His fresh theoretical proof was and still is considered by some writers to be invalid.<ref name="Siegel"/><ref name="Schirrmacher 2001"/>
 
But more importantly, it relied on a new theoretical postulate of '''"perfectly black bodies"''', which is the reason why one speaks of Kirchhoff's law. Such black bodies showed complete absorption in their infinitely thin most superficial surface. They correspond to Balfour Stewart's reference bodies, with internal radiation, coated with lamp-black. They were not the more realistic perfectly black bodies later considered by Planck. Planck's black bodies radiated and absorbed only by the material in their interiors; their interfaces with contiguous media were only mathematical surfaces, capable neither of absorption nor emission, but only of reflecting and transmitting with refraction.<ref>{{harvnb|Planck|1914|page=11}}</ref>
 
Kirchhoff's proof considered an arbitrary non-ideal body labeled {{math|''i''}} as well as various perfect black bodies labeled {{math|BB}} . It required that the bodies be kept in a cavity in thermal equilibrium at temperature {{math|''T''}} . His proof intended to show that the ratio {{math|''E''(''λ'', ''T'', ''i'') / ''a''(''λ'', ''T'', ''i'')}} was independent of the nature {{math|''i''}} of the non-ideal body, however partly transparent or partly reflective it was.
 
His proof first argued that for wavelength {{math|''λ''}} and at temperature {{math|''T''}}, at thermal equilibrium, all perfectly black bodies of the same size and shape have the one and the same common value of emissive power {{math|''E''(''λ'', ''T'', BB)}}, with the dimensions of power. His proof noted that the dimensionless wavelength-specific absorption ratio {{math|''a''(''λ'', ''T'', BB)}} of a perfectly black body is by definition exactly 1. Then for a perfectly black body, the wavelength-specific ratio of emissive power to absorption ratio {{math|''E''(''λ'', ''T'', BB) / ''a''(''λ'', ''T'', BB)}} is again just {{math|''E''(''λ'', ''T'', BB)}}, with the dimensions of power. Kirchhoff considered, successively, thermal equilibrium with the arbitrary non-ideal body, and with a perfectly black body of the same size and shape, in place in his cavity in equilibrium at temperature {{math|''T''}} . He argued that the flows of heat radiation must be the same in each case. Thus he argued that at thermal equilibrium the ratio {{math|''E''(''λ'', ''T'', ''i'') / ''a''(''λ'', ''T'', ''i'')}} was equal to {{math|''E''(''λ'', ''T'', BB)}}, which may now be denoted {{math|''B''<sub>''λ''</sub> (''λ'', ''T'')}}, a continuous function, dependent only on {{math|''λ''}} at fixed temperature {{math|''T''}}, and an increasing function of {{math|''T''}} at fixed wavelength {{math|''λ''}}, at low temperatures vanishing for visible but not for longer wavelengths, with positive values for visible wavelengths at higher temperatures, which does not depend on the nature {{math|''i''}} of the arbitrary non-ideal body. (Geometrical factors, taken into detailed account by Kirchhoff, have been ignored in the foregoing.)
 
Thus '''Kirchhoff's law of thermal radiation''' can be stated: ''For any material at all, radiating and absorbing in thermodynamic equilibrium at any given temperature {{math|T}}, for every wavelength {{math|λ}}, the ratio of emissive power to absorptive ratio has one universal value, which is characteristic of a perfect black body, and is an emissive power which we here represent by {{math|B<sub>λ</sub> (λ, T)}} .'' (For our notation {{math|''B''<sub>''λ''</sub> (''λ'', ''T'')}}, Kirchhoff's original notation was simply {{math|''e''}}.)<ref name="Chan8"/><ref name="Kirchhoff 1860c"/><ref>{{harvnb|Milne|1930|page=80}}</ref><ref>{{harvnb|Rybicki|Lightman|1979|pages=16–17}}</ref><ref>{{harvnb|Mihalas|Weibel-Mihalas|1984|page=328}}</ref><ref>{{harvnb|Goody|Yung|1989|pages=27–28}}</ref>
 
Kirchhoff announced that the determination of the function {{math|''B''<sub>''λ''</sub> (''λ'', ''T'')}} was a problem of the highest importance, though he recognized that there would be experimental difficulties to be overcome. He supposed that like other functions that do not depend on the properties of individual bodies, it would be a simple function. That function {{math|''B''<sub>''λ''</sub> (''λ'', ''T'')}} has occasionally been called 'Kirchhoff's (emission, universal) function',<ref>[[Friedrich Paschen|Paschen, F.]] (1896), personal letter cited by {{harvnb|Hermann|1971}}, p. 6</ref><ref>{{harvnb|Hermann|1971}}, p. 7</ref><ref>{{harvnb|Kuhn|1978|pages=8, 29}}</ref><ref>{{harvnb|Mehra and Rechenberg|1982|pages=26, 28, 31, 39}}</ref> though its precise mathematical form would not be known for another forty years, till it was discovered by Planck in 1900. The theoretical proof for Kirchhoff's universality principle was worked on and debated by various physicists over the same time, and later.<ref name="Schirrmacher 2001"/> Kirchhoff stated later in 1860 that his theoretical proof was better than Balfour Stewart's, and in some respects it was so.<ref name="Siegel"/> Kirchhoff's 1860 paper did not mention the second law of thermodynamics, and of course did not mention the concept of entropy which had not at that time been established. In a more considered account in a book in 1862, Kirchhoff mentioned the connection of his law with "Carnot's principle", which is a form of the second law.<ref>{{harvnb|Kirchhoff|1862/1882|page=573}}</ref>
 
According to Helge Kragh, "Quantum theory owes its origin to the study of thermal radiation, in particular to the "blackbody" radiation that Robert Kirchhoff had first defined in 1859–1860."<ref>{{harvnb|Kragh|1999|page=58}}</ref>
 
===Empirical sources of Planck's law===
 
In 1860, Kirchhoff predicted experimental difficulties for the empirical determination of the function that described the dependence of the black-body spectrum as a function only of temperature and wavelength. And so it turned out. It took some forty years of development of improved methods of measurement of electromagnetic radiation to get a reliable result.<ref name="Kangro 1976">{{harvnb|Kangro|1976}}</ref>
 
In 1865, [[John Tyndall]] described radiation from electrically heated filaments and from carbon arcs as visible and invisible.<ref>{{harvnb|Tyndall|1865a}}</ref> Tyndall spectrally decomposed the radiation by use of a rock salt prism, which passed heat as well as visible rays, and measured the radiation intensity by means of a thermopile.<ref>{{harvnb|Tyndall|1865b}}</ref><ref>{{harvnb|Kangro|1976|pages=8–10}}</ref>
 
In 1880, André-Prosper-Paul Crova published a diagram of the three-dimensional appearance of the graph of the strength of thermal radiation as a function of wavelength and temperature.<ref>{{harvnb|Crova|1880}}</ref>
 
In a series of papers from 1881 to 1886, Langley reported measurements of the spectrum of heat radiation, using diffraction gratings and prisms, and the most sensitive detectors that he could make. He reported that there was a peak intensity that increased with temperature, that the shape of the spectrum was not symmetrical about the peak, that there was a strong fall-off of intensity when the wavelength was shorter than an approximate cut-off value for each temperature, that the approximate cut-off wavelength decreased with increasing temperature, and that the wavelength of the peak intensity decreased with temperature, so that the intensity increased strongly with temperature for short wavelengths that were longer than the approximate cut-off for the temperature.<ref>{{harvnb|Kangro|1976|pages=15–26}}</ref>
 
In 1898, [[Otto Lummer]] and [[Ferdinand Kurlbaum]] published an account of their cavity radiation source.<ref>{{harvnb|Lummer|Kurlbaum|1898}}</ref> Their design has been used largely unchanged for radiation measurements to the present day. It was a platinum box, divided by diaphragms, with its interior blackened with iron oxide. It was an important ingredient for the progressively improved measurements that led to the discovery of Planck's law.<ref>{{harvnb|Kangro|1976|page=159}}</ref> A version described in 1901 had its interior blackened with a mixture of chromium, nickel, and cobalt oxides.<ref>{{harvnb|Lummer|Kurlbaum|1901}}</ref>
 
The importance of the Lummer and Kurlbaum cavity radiation source was that it was an experimentally accessible source of black-body radiation, as distinct from radiation from a simply exposed incandescent solid body, which previously was the nearest available experimental approximation to black-body radiation over a suitable range of temperatures. The simply exposed incandescent solid bodies, that had previously been used, emitted radiation with departures from the black-body spectrum that made it impossible to find the true black-body spectrum from experiments.<ref>{{harvnb|Kangro|1976|[pages= 75–76}}</ref><ref>{{harvnb|Paschen|1895|pages=297–301}}</ref>
 
===Planck's views just before the empirical facts led him to find his eventual law===
 
Theoretical and empirical progress enabled Lummer and Pringsheim to write in 1899 that available experimental evidence was approximately consistent with the specific intensity law {{math|''Cλ<sup>−5</sup>e<sup>(−c/λT)</sup>''}} where {{math|''C''}} and {{math|''c''}} denote empirically measurable constants, and where {{math|''λ''}} and {{math|''T''}} denote wavelength and temperature respectively.<ref>{{harvnb|Lummer|Pringsheim|1899|page=225}}</ref><ref>{{harvnb|Kangro|1976|page=174}}</ref> For theoretical reasons, Planck at that time accepted this formulation, which has an effective cut-off of short wavelengths.<ref name="Planck 1900d">{{harvnb|Planck|1900d}}</ref><ref name="Rayleigh 1900 539">{{harvnb|Rayleigh|1900|page=539}}</ref><ref name="Kangro 1976 181">{{harvnb|Kangro|1976|pages=181–183}}</ref>
 
===Finding the empirical law===
[[Max Planck]] originally produced his law on 19 October 1900<ref name="Planck 1900a">{{harvnb|Planck|1900a}}</ref><ref name="Planck 1900b">{{harvnb|Planck|1900b}}</ref> as an improvement upon the [[Wien approximation]], published in 1896 by [[Wilhelm Wien]], which fit the experimental data at short wavelengths (high frequencies) but deviated from it at long wavelengths (low frequencies).<ref name="Wien 1896 667"/> In June 1900, based on heuristic theoretical considerations, Rayleigh had suggested a formula<ref name="Rayleigh 1900">{{harvnb|Rayleigh|1900}}</ref> that he proposed might be checked experimentally. The suggestion was that the Stewart–Kirchhoff universal function might be of the form <math>c_1T\lambda^{-4}\mathrm{exp}(-c_2/\lambda T)</math> . This was not the celebrated Rayleigh–Jeans formula <math>8\pi k_{\mathrm{B}}T\lambda^{-4}</math>, which did not emerge until 1905,<ref name="Jeans 1905a"/> though it did reduce to the latter for long wavelengths, which are the relevant ones here. According to Klein,<ref name="Klein 1962">{{harvnb|Klein|1962}}</ref> one may speculate that it is likely that Planck had seen this suggestion though he did not mention it in his papers of 1900 and 1901. Planck would have been aware of various other proposed formulas which had been offered.<ref name="Kangro 1976"/><ref name="Dougal">{{harvnb|Dougal|1976}}</ref> On 7 October 1900, Rubens told Planck that in the complementary domain (long wavelength, low frequency), and only there, Rayleigh's 1900 formula fitted the observed data well.<ref name="Dougal"/>
 
For long wavelengths, Rayleigh's 1900 heuristic formula approximately meant that energy was proportional to temperature, {{math|''U'' {{=}} const. ''T''}}.<ref name="Klein 1962"/><ref name="Dougal"/><ref>{{harvnb|Planck|1943|page=156}}</ref> It is known that <math>\mathrm{d}S/\mathrm{d}U=1/T</math> and this leads to <math>\mathrm{d}S/\mathrm{d}U=\mathrm{const.}/ U</math> and thence to {{math|d<sup>2</sup>''S'' /d''U''<sup> 2</sup> {{=}} − const. / ''U''<sup> 2</sup>}}  for long wavelengths. But for short wavelengths, the Wien formula leads to {{math|1 / ''T'' {{=}} − const. / ln ''U'' + const.}} and thence to {{math|d<sup>2</sup>''S'' /d''U''<sup> 2</sup> {{=}} − const. / ''U''}} for short wavelengths. Planck perhaps patched together these two heuristic formulas, for long and for short wavelengths,<ref name="Dougal"/><ref>{{harvnb|Hettner|1922}}</ref> to produce a formula
:<math>\mathrm{d}^2 S/\mathrm{d}U^2=\frac{\alpha}{U(\beta+U)}.</math><ref name="Planck 1900a"/>
 
This led Planck to the formula
:<math>B_\lambda(T) =\frac{C\lambda^{-5}}{e^{\frac{c}{\lambda T}} - 1},</math>
 
where Planck used the symbols <math>C</math> and <math>c</math> to denote empirical fitting constants.
 
Planck sent this result to Rubens, who compared it with his and Kurlbaum's observational data and found that it fitted for all wavelengths remarkably well. On 19 October 1900, Rubens and Kurlbaum briefly reported the fit to the data,<ref>{{harvnb|Rubens|Kurlbaum|1900a}}</ref> and Planck added a short presentation to give a theoretical sketch to account for his formula.<ref name="Planck 1900a"/> Within a week, Rubens and Kurlbaum gave a fuller report of their measurements confirming Planck's law. Their technique for spectral resolution of the longer wavelength radiation was called the residual ray method. The rays were repeatedly reflected from polished crystal surfaces, and the rays that made it all the way through the process were 'residual', and were of wavelengths preferentially reflected by crystals of suitably specific materials.<ref>{{harvnb|Rubens|Kurlbaum|1900b}}</ref><ref>{{harvnb|Kangro|1976|page=165}}</ref><ref>{{harvnb|Mehra|Rechenberg|1982|page=41}}</ref>
 
===Trying to find a physical explanation of the law===
Once Planck had discovered the empirically fitting function, he constructed a physical derivation of this law. His thinking revolved around entropy rather than being directly about temperature. Planck considered a cavity with perfectly reflective walls; the cavity contained finitely many hypothetical well separated and recognizable but identically constituted, of definite magnitude, resonant oscillatory bodies, several such oscillators at each of finitely many characteristic frequencies. The hypothetical oscillators were for Planck purely imaginary theoretical investigative probes, and he said of them that such oscillators do not need to "really exist somewhere in nature, provided their existence and their properties are consistent with the laws of thermodynamics and electrodynamics.".<ref>{{harvnb|Planck|1914|p=135}}</ref> Planck did not attribute any definite physical significance to his hypothesis of resonant oscillators, but rather proposed it as a mathematical device that enabled him to derive a single expression for the black body spectrum that matched the empirical data at all wavelengths.<ref>{{harvnb|Kuhn|1978|pages=117–118}}</ref> He tentatively mentioned the possible connection of such oscillators with atoms. In a sense, the oscillators corresponded to Planck's speck of carbon; the size of the speck could be small regardless of the size of the cavity, provided the speck effectively transduced energy between radiative wavelength modes.<ref name="Dougal"/>
 
Partly following a heuristic method of calculation pioneered by Boltzmann for gas molecules, Planck considered the possible ways of distributing electromagnetic energy over the different modes of his hypothetical charged material oscillators. This acceptance of the probabilistic approach, following Boltzmann, for Planck was a radical change from his former position, which till then had deliberately opposed such thinking proposed by Boltzmann.<ref>{{harvnb|Hermann|1971}}, p. 16</ref> Heuristically, Boltzmann had distributed the energy in arbitrary merely mathematical quanta  ''ϵ'', which he had proceeded to make tend to zero in magnitude, because the finite magnitude ''ϵ'' had served only to allow definite counting for the sake of mathematical calculation of probabilities, and had no physical significance. Referring to a new universal constant of nature, ''h'',<ref>{{harvnb|Planck|1900c}}</ref> Planck supposed that, in the several oscillators of each of the finitely many characteristic frequencies, the total energy was distributed to each in an integer multiple of a definite physical unit of energy, ''ϵ'', not arbitrary as in Boltzmann's method, but now for Planck, in a new departure, characteristic of the respective characteristic frequency.<ref name="Planck 1900b"/><ref>{{harvnb|Kangro|1976|p=214}}</ref><ref>{{harvnb|Kuhn|1978|p=106}}</ref><ref name="Kraghe">{{harvnb|Kragh|2000}}</ref> His new universal constant of nature, ''h'', is now known as [[Planck's constant]].
 
Planck explained further<ref name="Planck 1900b"/> that the respective definite unit, ''ϵ'', of energy should be proportional to the respective characteristic oscillation frequency <math>\nu</math> of the hypothetical oscillator, and in 1901 he expressed this with the constant of proportionality ''h'':<ref name="planck">{{harvnb|Planck|1901}}</ref><ref>{{harvnb|Planck|1915|p=89}}</ref>
:<math>\epsilon=h\nu.</math>
This is known as [[Planck's relation]].<ref>{{harvnb|Schumm|2004|p=34}}</ref>
 
Planck did not propose that light propagating in free space is quantized.<ref>{{harvnb|Ehrenfest|Kamerlingh Onnes|1914|page=873}}</ref><ref>{{harvnb|ter Haar|1967|p=14}}</ref><ref>{{harvnb|Stehle|1994|p=128}}</ref> The idea of quantization of the free electromagnetic field was developed later, and eventually incorporated into what we now know as [[quantum field theory]].<ref>{{harvnb|Scully|Zubairy|1997|page=21}}.</ref>
 
In 1906 Planck acknowledged that his imaginary resonators, having linear dynamics, did not provide a physical explanation for energy transduction between frequencies.<ref>{{harvnb|Planck|1906|page=220}}</ref><ref>{{harvnb|Kuhn|1978|page=162}}</ref> Present-day physics explains the transduction between frequencies in the presence of atoms by their quantum excitability, following Einstein. Planck believed that in a cavity with perfectly reflecting walls and with no matter present, the electromagnetic field cannot exchange energy between frequency components.<ref name="Planck 1914a">{{harvnb|Planck|1914|pp=44–45, 113–114}}</ref> This is because of the [[Linear#Physics|linearity]] of [[Maxwell's equations]].<ref name="Stehle 150"/> Present-day quantum field theory predicts that, in the absence of matter, the electromagnetic field obeys [[Euler-Heisenberg Lagrangian|nonlinear]] equations and in that sense does self-interact.<ref name="Jauch Rohrlich">{{harvnb|Jauch|Rohrlich|1980}}, Chapter 13</ref><ref name=Karplus>Robert Karplus* and Maurice Neuman,"The Scattering of Light by Light", Phys. Rev. 83, 776–784 (1951)</ref> Such interaction in the absence of matter has not yet been directly measured because it would require very high intensities and very sensitive and low-noise detectors, which are still in the process of being constructed.<ref name="Jauch Rohrlich"/><ref>{{cite journal | last1 = Tommasini | first1 = D. | last2 = Ferrando | first2 = F. | last3 = Michinel | first3 = H. | last4 = Seco | first4 = M. | year = 2008 | title = Detecting photon-photon scattering in vacuum at exawatt lasers | url = | journal = Phys. Rev. A | volume = 77 | issue = | page = 042101 |arxiv = quant-ph/0703076 |bibcode = 2008PhRvA..77a2101M |doi = 10.1103/PhysRevA.77.012101 }}</ref>  Planck believed that a field with no interactions neither obeys nor violates the classical principle of equipartition of energy,<ref>{{harvnb|Jeffreys|1973|p=223}}</ref><ref>{{harvnb|Planck|1906|page=178}}</ref> and instead remains exactly as it was when introduced, rather than evolving into a black body field.<ref>{{harvnb|Planck|1914|page=26}}</ref> Thus, the linearity of his mechanical assumptions precluded Planck from having a mechanical explanation of the maximization of the entropy of the thermodynamic equilibrium thermal radiation field. This is why he had to resort to Boltzmann's probabilistic arguments.<ref>{{harvnb|Boltzmann|1878}}</ref><ref>{{harvnb|Kuhn|1978|pages=38–39}}</ref>
 
Planck's law may be regarded as fulfulling the prediction of [[Gustav Kirchhoff]] that his [[Kirchhoff's law of thermal radiation|law of thermal radiation]] was of the highest importance. In his mature presentation of his own law, Planck offered a thorough and detailed theoretical proof for Kirchhoff's law,<ref>{{harvnb|Planck|1914|pages =1–45}}</ref> theoretical proof of which until then had been sometimes debated, partly because it was said to rely on unphysical theoretical objects, such as Kirchhoff's perfectly absorbing infinitely thin black surface.<ref>{{harvnb|Cotton|1899}}</ref>
 
===Subsequent events===
 
It was not till five years after Planck made his heuristic assumption of abstract elements of energy or of action that [[Albert Einstein]] conceived of really existing [[Quantum|quanta]] of light in 1905<ref name="Einstein 1905">{{harvnb|Einstein|1905}}</ref> as a revolutionary explanation of black-body radiation, of photoluminescence, of the [[photoelectric effect]], and of the ionization of gases by ultraviolet light. In 1905, "Einstein believed that Planck's theory could not be made to agree with the idea of light quanta, a mistake he corrected in 1906."<ref>{{harvnb|Kragh|1999|page=67}}</ref> Contrary to Planck's beliefs of the time, Einstein proposed a model and formula whereby light was emitted, absorbed, and propagated in free space in energy quanta localized in points of space.<ref name="Einstein 1905"/> As an introduction to his reasoning, Einstein recapitulated Planck's model of hypothetical resonant material electric oscillators as sources and sinks of radiation, but then he offered a new argument, disconnected from that model, but partly based on a thermodynamic argument of Wien, in which Planck's formula ''ϵ'' = <math>h\nu</math> played no role.<ref name="Stehle 132–137">{{harvnb|Stehle|1994|pages=132–137}}</ref> Einstein gave the energy content of such quanta in the form <math>R\beta\nu/N</math>. Thus Einstein was contradicting the undulatory theory of light held by Planck. In 1910, criticizing a manuscript sent to him by Planck, knowing that Planck was a steady supporter of Einstein's theory of special relativity, Einstein wrote to Planck: "To me it seems absurd to have energy continuously distributed in space without assuming an aether."<ref>{{harvnb|Einstein|1993|page=143}}, letter of 1910.</ref>
 
According to Thomas Kuhn, it was not till 1908 that Planck more or less accepted part of Einstein's arguments for physical as distinct from abstract mathematical discreteness in thermal radiation physics. Still in 1908, considering Einstein's proposal of quantal propagation, Planck opined that such a revolutionary step was perhaps unnecessary.<ref>{{harvnb|Planck|1915|p=95}}</ref> Until then, Planck had been consistent in thinking that discreteness of action quanta was to be found neither in his resonant oscillators nor in the propagation of thermal radiation. Kuhn wrote that, in Planck's earlier papers and in his 1906 monograph,<ref name="Planck 1906">{{harvnb|Planck|1906}}</ref> there is no "mention of discontinuity, [nor] of talk of a restriction on oscillator energy,  [nor of] any formula like {{math|''U'' {{=}} ''nhν''}}."<ref>{{harvnb|Kuhn|1984|page=236}}</ref> Kuhn pointed out that his study of Planck's papers of 1900 and 1901, and of his monograph of 1906,<ref name="Planck 1906"/> had led him to "heretical" conclusions, contrary to the widespread assumptions of others who saw Planck's writing only from the perspective of later, anachronistic, viewpoints.<ref>{{harvnb|Kuhn|1978|pages=196–202}}</ref><ref>{{harvnb|Kuhn|1984}}</ref> Kuhn's conclusions, finding a period till 1908, when Planck consistently held his 'first theory', have been accepted by other historians.<ref>{{harvnb|Darrigol|1992|page=76}}</ref><ref>{{harvnb|Kragh|1999|pages=63–66}}</ref>
 
In the second edition of his monograph, in 1912, Planck sustained his dissent from Einstein's proposal of light quanta. He proposed in some detail that absorption of light by his virtual material resonators might be continuous, occurring at a constant rate in equilibrium, as distinct from quantal absorption. Only emission was quantal.<ref name="Stehle 150">{{harvnb|Stehle|1994|p=150}}</ref><ref>{{harvnb|Planck|1914|p=161}}</ref> This has at times been called Planck's "second theory".<ref>{{harvnb|Kuhn|1978|pages=235–253}}</ref>
 
It was not till 1919 that Planck in the third edition of his monograph more or less accepted his 'third theory', that both emission and absorption of light were quantal.<ref>{{harvnb|Kuhn|1978|pages=253–254}}</ref>
 
The colourful term "[[ultraviolet catastrophe]]" was given by [[Paul Ehrenfest]] in 1911 to the paradoxical result that the total energy in the cavity tends to infinity when the [[equipartition theorem]] of classical statistical mechanics is (mistakenly) applied to black body radiation.<ref>{{harvnb|Ehrenfest|1911}}</ref><ref>{{harvnb|Kuhn|1978|page=152}}</ref> But this had not been part of Planck's thinking, because he had not tried to apply the doctrine of equipartition: when he made his discovery in 1900, he had not noticed any sort of "catastrophe".<ref name="Planck 1900d"/><ref name="Rayleigh 1900 539"/><ref name="Kangro 1976 181"/><ref name="Klein 1962"/><ref>{{harvnb|Kuhn|1978|pages = 151–152}}</ref> It was first noted by [[Lord Rayleigh]] in 1900,<ref name="Rayleigh 1900"/><ref>{{harvnb|Kangro|1976|page=190}}</ref><ref>{{harvnb|Kuhn|1978|pages = 144–145}}</ref> and then in 1901<ref>See footnote on p. 398 in {{harvnb|Jeans|1901}}</ref> by Sir [[James Jeans]]; and later, in 1905, by Einstein when he wanted to support the idea that light propagates as discrete packets, later called 'photons', and by Rayleigh<ref name="Rayleigh 1905"/> and by Jeans.<ref name="Jeans 1905a"/><ref>{{harvnb|Jeans|1905b}}</ref><ref>{{harvnb|Jeans|1905c}}</ref><ref>{{harvnb|Jeans|1905d}}</ref>
 
In 1913, Bohr gave another formula with a further different physical meaning to the quantity {{math|''hν''}}.<ref name="Einstein 1916">{{harvnb|Einstein|1916}}</ref><ref name="Bohr 1913">{{harvnb|Bohr|1913}}</ref><ref name="Jammer 1989 113 115">{{harvnb|Jammer|1989|pages=113, 115}}</ref><ref name="Sommerfeld 1923 43">{{harvnb|Sommerfeld|1923|p=43}}</ref><ref name ="Heisenberg 1925 108">{{harvnb|Heisenberg|1925|p=108}}</ref><ref name="Brillouin 1970 31">{{harvnb|Brillouin|1970|p=31}}</ref> In contrast to Planck's and Einstein's formulas, Bohr's formula referred explicitly and categorically to energy levels of atoms. Bohr's formula was <math>W_{\tau_2} - W_{\tau_1}=h\nu</math> where <math>W_{\tau_2}</math> and <math>W_{\tau_1}</math> denote the energy levels of quantum states of an atom, with quantum numbers <math>\tau_2\ </math> and <math>\tau_1\ </math>. The symbol <math>\nu\ </math> denotes the frequency of a quantum of radiation that can be emitted or absorbed as the atom passes between those two quantum states. In contrast to Planck's model, the frequency <math>\nu\ </math> has no immediate relation to frequencies that might describe those quantum states themselves.
 
Later, in 1924, [[Satyendra Nath Bose]] developed the theory of the statistical mechanics of photons, which allowed a [[gas in a box|theoretical derivation]] of Planck's law. The actual word 'photon' was invented still later, by G.N. Lewis in 1926,<ref>{{harvnb|Lewis|1926}}</ref> who mistakenly believed that photons were conserved, contrary to Bose–Einstein statistics; nevertheless the word 'photon' was adopted to express the Einstein postulate of the packet nature of light propagation. In an electromagnetic field isolated in a vacuum in a vessel with perfectly reflective walls, such as was considered by Planck, indeed the photons would be conserved according to Einstein's 1905 model, but Lewis was referring to a field of photons considered as a system closed with respect to ponderable matter but open to exchange of electromagnetic energy with a surrounding system of ponderable matter, and he mistakenly imagined that still the photons were conserved, being stored inside atoms.
 
Ultimately, Planck's law of black-body radiation contributed to Einstein's concept of quanta of light carrying linear momentum,<ref name="Einstein 1916"/><ref name="Einstein 1905"/> which became the fundamental basis for the development of [[quantum mechanics]].
 
The above-mentioned linearity of Planck's mechanical assumptions, not allowing for energetic interactions between frequency components, was superseded in 1925 by Heisenberg's original quantum mechanics. In his paper submitted on 29 July 1925, Heisenberg's theory accounted for Bohr's above-mentioned formula of 1913. It admitted non-linear oscillators as models of atomic quantum states, allowing energetic interaction between their own multiple internal discrete Fourier frequency components, on the occasions of emission or absorption of quanta of radiation. The frequency of a quantum of radiation was that of a definite coupling between internal atomic meta-stable oscillatory quantum states.<ref>{{harvnb|Heisenberg|1925}}</ref><ref>{{harvnb|Razavy|2011|pages=39–41}}</ref> At that time, Heisenberg knew nothing of matrix albegra, but [[Max Born]] read the manuscript of Heisenberg's paper and recognized the matrix character of Heisenberg's theory. Then Born and [[Pascual Jordan|Jordan]] published an explicitly matrix theory of quantum mechanics, based on, but in form distinctly different from, Heisenberg's original quantum mechanics; it is the Born and Jordan matrix theory that is today called matrix mechanics.<ref>{{harvnb|Born|Jordan|1925}}</ref><ref>{{harvnb|Stehle|1994|page=286}}</ref><ref>{{harvnb|Razavy|2011|pages=42–43}}</ref> Heisenberg's explanation of the Planck oscillators, as non-linear effects apparent as Fourier modes of transient processes of emission or absorption of radiation, showed why Planck's oscillators, viewed as enduring physical objects such as might be envisaged by classical physics, did not give an adequate explanation of the phenomena.
 
Nowadays, as a statement of the energy of a light quantum, often one finds the formula ''E'' = ''ħω'', where ''ħ'' = ''h''/2π, and ''ω'' = <math>2\pi\nu</math> denotes angular frequency,<ref>{{harvnb|Messiah|1958|p=14}}</ref><ref>{{harvnb|Pauli|1973|p=1}}</ref><ref>{{harvnb|Feynman|Leighton|Sands|1963|p=38-1<!--Lectures on Physics uses a nonstandard page number scheme. These comments will prevent bots from adding a dash when a hyphen is meant-->}}</ref><ref name="Schwinger 2001 203"/><ref name="BC 2006 2"/> and less often the equivalent formula ''E'' = <math>h\nu</math>.<ref name="Schwinger 2001 203">{{harvnb|Schwinger|2001|p=203}}</ref><ref name="BC 2006 2">{{harvnb|Bohren|Clothiaux|2006|p=2}}</ref><ref>{{harvnb|Schiff|1949|p=2}}</ref><ref>{{harvnb|Mihalas|Weibel-Mihalas|1984|p=143}}</ref><ref>{{harvnb|Rybicki|Lightman|1979|p=20}}</ref> This statement about a really existing and propagating light quantum, based on Einstein's, has a physical meaning different from that of Planck's above statement ''ϵ'' = <math>h\nu</math> about the abstract energy units to be distributed amongst his hypothetical resonant material oscillators.
 
An article by Helge Kragh published in ''[[Physics World]]'' gives an account of this history.<ref name="Kraghe"/>
 
==See also==
* [[Radiance]]
* [[Sakuma–Hattori equation]]
 
==References==
{{reflist|colwidth=30em}}
 
=== Bibliography ===
{{refbegin}}
*{{cite journal
|last1=Bohr |first1=N.
|author1-link=Niels Bohr
|year=1913
|title=On the constitution of atoms and molecules
|url=http://www.ffn.ub.es/luisnavarro/nuevo_maletin/Bohr_1913.pdf | doi = 10.1080/14786441308634993
|journal=[[Philosophical Magazine]]
|volume=26 |pages=1–25
|ref=harv
}}
*{{cite book
|last1=Bohren |first1=C. F.
|author1-link=Craig Bohren
|last2=Clothiaux |first2=E. E.
|year=2006
|title=Fundamentals of Atmospheric Radiation
|publisher=[[Wiley-VCH]]
|isbn=3-527-40503-8
|ref=harv
}}
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|author1-link=Ludwig Boltzmann
|year=1878
|title=Über die Beziehung zwischen dem zweiten Hauptsatze der mechanischen Wärmetheorie und der Wahrscheinlichkeitsrechnung, respective den Sätzen über das Wärmegleichgewicht
|journal=[[Sitzungsberichte Mathematisch-Naturwissenschaftlichen Classe der kaiserlichen Akademie der Wissenschaften in Wien]]
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|title=Zur Quantenmechanik
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|volume=34
|pages=858–888
|bibcode=1925ZPhy...34..858B
|doi=10.1007/BF01328531
|ref=harv
}} Translated in part as "On quantum mechanics" in {{cite book
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|author1-link=Paul Ehrenfest
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|volume=36 |pages=91–118
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*{{cite journal
|last1=Einstein |first1=A.
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|title=Über einen die Erzeugung und Verwandlung des Lichtes betreffenden heuristischen Gesichtspunkt
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|journal=[[Annalen der Physik]]
|volume=17 |issue=6 |pages=132–148
|bibcode=1905AnP...322..132E
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|year=1965
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*{{cite journal
|last1=Einstein |first1=A.
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|title=Zur Quantentheorie der Strahlung
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|volume=18 |pages=47–62
|ref=harv
}} and a nearly identical version {{cite journal
|last1=Einstein |first1=A.
|author1-link=Albert Einstein
|year=1917
|title=Zur Quantentheorie der Strahlung
|journal=[[Physikalische Zeitschrift]]
|volume=18 |pages=121–128
|bibcode=1917PhyZ...18..121E
|ref=harv
}} Translated in {{cite book
|last1=ter Haar |first1=D.
|author-link=Dirk ter Haar
|year=1967
|pages=167–183
|title=The Old Quantum Theory
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|lccn=66029628
|ref=harv
}} See also [http://astro1.panet.utoledo.edu/~ljc/einstein_ab.pdf].
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|title=Über quantentheoretische Umdeutung kinematischer und mechanischer Beziehungen
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|volume=33
|pages=879–893
|bibcode=1925ZPhy...33..879H
|doi=10.1007/BF01328377
|ref=harv
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|author1-link=Bartel Leendert van der Waerden
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  |ref=harv
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  |isbn=0-262-08047-8
  |ref=harv
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}}
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|year=1967
|chapter=On the Theory of the Energy Distribution Law of the Normal Spectrum
|url=http://www.ffn.ub.es/luisnavarro/nuevo_maletin/Planck%20%281900%29,%20Distribution%20Law.pdf
|title=The Old Quantum Theory
|publisher=[[Pergamon Press]]
|page=82
|lccn=66029628
}}
*{{cite journal
|last1=Planck |first1=M.
|author1-link=Max Planck
|year=1900c
|title=Entropie und Temperatur strahlender Wärme
|journal=[[Annalen der Physik]]
|volume=306 |issue=4 |pages=719–737
|bibcode=1900AnP...306..719P
|doi=10.1002/andp.19003060410
|ref=harv
}}
*{{cite journal
|last1=Planck |first1=M.
|author1-link=Max Planck
|year=1900d
|title=Über irreversible Strahlungsvorgänge
|journal=[[Annalen der Physik]]
|volume=306
|issue=1
|pages=69–122
|bibcode=1900AnP...306...69P
|doi=10.1002/andp.19003060105
|ref=harv
}}
*{{cite journal
|last1=Planck |first1=M.
|author1-link=Max Planck
|year=1901
|title=Über das Gesetz der Energieverteilung im Normalspektrum
|journal=[[Annalen der Physik]]
|volume=4 |page=553
|ref=harv
}} Translated in {{cite web
|last1=Ando |first1=K.
|year=
|title=On the Law of Distribution of Energy in the Normal Spectrum
|url=http://theochem.kuchem.kyoto-u.ac.jp/Ando/planck1901.pdf
|accessdate=13 October 2011
}}
*{{cite book
|last1=Planck |first1=M.
|author1-link=Max Planck
|year=1906
|title=Vorlesungen über die Theorie der Wärmestrahlung
|publisher=[[Johann Ambrosius Barth]]
|ref=harv
|lccn=07004527
}}
*{{cite book
|last1=Planck |first1=M.
|author1-link=Max Planck
|others=Masius, M. (transl.)
|year=1914
|title=The Theory of Heat Radiation
|publisher=[[P. Blakiston's Son & Co.|P. Blakiston's Son & Co]]
|edition=2nd
|ol=7154661M
|ref=harv
}}
*{{cite book
|last1=Planck |first1=M.
|author1-link=Max Planck
|others=Wills, A. P. (transl.)
|year=1915
|title=Eight Lectures on Theoretical Physics
|publisher=[[Dover Publications]]
|isbn=0-486-69730-4
|ref=harv
}}
*{{cite journal
|last1=Planck |first1=M.
|author1-link=Max Planck
|year=1943
|title=Zur Geschichte der Auffindung des physikalischen Wirkungsquantums
|journal=[[Naturwissenschaften]]
|volume=31 |issue=14–15 |pages=153–159
|bibcode=1943NW.....31..153P
|doi=10.1007/BF01475738
|ref=harv
}}
*{{Cite journal
|last1=Rayleigh |first1=Lord
|author1-link=John Strutt, 3rd Baron Rayleigh
|year=1900
|title=LIII. Remarks upon the law of complete radiation
|journal=[[Philosophical Magazine]]
|series=Series 5 |volume=49 |issue=301 |page=539
|doi=10.1080/14786440009463878
|ref=harv
}}
*{{cite journal
|last1=Rayleigh |first1=Lord
|author1-link=John Strutt, 3rd Baron Rayleigh
|year=1905
|title=The Dynamical Theory of Gases and of Radiation
|journal=[[Nature (journal)|Nature]]
|volume=72 |issue=1855 |pages=54–55
|bibcode=1905Natur..72...54R
|doi=10.1038/072054c0
|ref=harv
}}
*{{cite book
|last1=Razavy |first1=M.
|author1-link=Mohshen Razavy
|year=2011
|title=Heisenberg's Quantum Mechanics
|publisher=[[World Scientific]]
|isbn=978-981-4304-10-8
|ref=harv
}}
*{{cite journal
|last1=Rubens |first1=H.
|author1-link=Heinrich Rubens
|last2=Kurlbaum |first2=F.
|author2-link=Ferdinand Kurlbaum
|year=1900a
|title=Über die Emission langer Wellen durch den schwarzen Körper
|journal=[[Verhandlungen der Deutschen Physikalischen Gesselschaft]]
|volume=2 |page=181
|ref=harv
}}
*{{cite journal
|last1=Rubens |first1=H.
|author1-link=Heinrich Rubens
|last2=Kurlbaum |first2=F.
|author2-link=Ferdinand Kurlbaum
|year=1900b
|title=Über die Emission langwelliger Wärmestrahlen durch den schwarzen Körper bei verschiedenen Temperaturen
|journal=[[Sitzungsberichte der Königlich Preussischen Akademie der Wissenschaften zu Berlin]]
|pages=929–941
|ref=harv
}} Translated in {{cite journal
|last1=Rubens |first1=H.
|author1-link=Heinrich Rubens
|last2=Kurlbaum |first2=F.
|author2-link=Ferdinand Kurlbaum
|year=1901
|title=On the heat-radiation of long wave-length emitted by black bodies at different temperatures
|journal=[[The Astrophysical Journal]]
|volume=14
|pages=335–348
|bibcode=1901ApJ....14..335R
|doi=10.1086/140874
|ref=harv
}}
*{{Cite book
|last1=Rybicki |first1=G. B.
|last2=Lightman |first2=A. P.
|author2-link=Alan Lightman
|year=1979
|title=Radiative Processes in Astrophysics
|url=http://books.google.com/books?id=LtdEjNABMlsC&printsec=frontcover
|publisher=[[John Wiley & Sons]]
|isbn=0-471-82759-2
|ref=harv
}}
*{{cite book
|last1=Sharkov |first1=E. A.
|year=2003
|chapter=Black-body radiation
|title=Passive Microwave Remote Sensing of the Earth
|url=http://www.iki.rssi.ru/asp/pub_sha1/Sharch06.pdf
|publisher=[[Springer (publisher)|Springer]]
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*{{cite book
|last1=Schiff|first1=L. I.
|author1-link=Leonard I. Schiff
|year=1949
|title=Quantum Mechanics
|publisher=[[McGraw-Hill]]
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*{{cite book
|last1=Schirrmacher |first1=A.
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|title=Experimenting theory: the proofs of Kirchhoff's radiation law before and after Planck
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*{{cite book
|last1=Schwinger |first1=J.
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*{{cite book
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*{{cite journal
|last1=Siegel |first1=D.M.
|year=1976
|title=Balfour Stewart and Gustav Robert Kirchhoff: two independent approaches to "Kirchhoff's radiation law"
|journal=[[Isis]]
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*{{cite book
|last1=Sommerfeld |first1=A.
|others=Brose, H. L. (transl.)
|author1-link=Arnold Sommerfeld
|year=1923
|title=Atomic Structure and Spectral Lines
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*{{cite book
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*{{cite journal
|last1=Stewart |first1=B.
|author1-link=Balfour Stewart
|year=1858
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*{{cite journal
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|year=1865b
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*{{cite journal
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|author1-link=Wilhelm Wien
|year=1896
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}}
{{refend}}
 
==External links==
* [http://topex.ucsd.edu/rs/radiation.pdf Summary of Radiation]
* [http://www.vias.org/simulations/simusoft_blackbody.html Radiation of a Blackbody] – interactive simulation to play with Planck's law
* [http://scienceworld.wolfram.com/physics/PlanckLaw.html Scienceworld entry on Planck's Law]
 
{{Use dmy dates|date=September 2010}}
 
{{DEFAULTSORT:Planck's Law}}
[[Category:Statistical mechanics]]
[[Category:Foundational quantum physics]]
 
[[ar:قانون بلانك]]
[[be:Формула Планка]]
[[bg:Закон на Планк]]
[[ca:Llei de Planck]]
[[cs:Planckův vyzařovací zákon]]
[[de:Plancksches Strahlungsgesetz]]
[[et:Plancki kiirgusseadus]]
[[es:Ley de Planck]]
[[eo:Leĝo de Planck]]
[[fa:قانون پلانک]]
[[fr:Loi de Planck]]
[[ko:플랑크 법칙]]
[[hr:Planckov zakon]]
[[it:Legge di Planck]]
[[mn:Планкийн хууль]]
[[nl:Wet van Planck]]
[[ja:プランクの法則]]
[[no:Plancks strålingslov]]
[[nn:Plancklova]]
[[pt:Lei de Planck]]
[[ro:Formula lui Planck]]
[[ru:Формула Планка]]
[[sl:Planckov zakon]]
[[sr:Планков закон]]
[[fi:Planckin laki mustan kappaleen säteilystä]]
[[th:กฎของพลังค์]]
[[zh:普朗克黑体辐射定律]]

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