Black-body radiation is thethermalelectromagnetic radiation within, or surrounding, a body inthermodynamic equilibrium with its environment, emitted by ablack body (an idealized opaque, non-reflective body). It has a specificcontinuous spectrum that depends only on the body'stemperature.[1][2][3][4]
A perfectly-insulated enclosure which is in thermal equilibrium internally contains blackbody radiation and will emit it through a hole made in its wall, provided the hole is small enough to have a negligible effect upon the equilibrium. The thermal radiation spontaneously emitted by many ordinary objects can be approximated as blackbody radiation.
Of particular importance, although planets and stars (including theEarth andSun) are neither in thermal equilibrium with their surroundings nor perfect black bodies, blackbody radiation is still a good first approximation for the energy they emit.[5]
The termblack body was introduced byGustav Kirchhoff in 1860.[6] Blackbody radiation is also calledthermal radiation,cavity radiation,complete radiation ortemperature radiation.
Black-body radiation has a characteristic, continuousfrequency spectrum that depends only on the body's temperature,[8] called the Planck spectrum orPlanck's law. The spectrum is peaked at a characteristic frequency that shifts to higher frequencies with increasing temperature, and atroom temperature most of the emission is in theinfrared region of theelectromagnetic spectrum.[9][10][11] As the temperature increases past about 500 degreesCelsius, black bodies start to emit significant amounts of visible light. Viewed in the dark by the human eye, the first faint glow appears as a "ghostly" grey (the visible light is actually red, but low intensity light activates only the eye's grey-level sensors). With rising temperature, the glow becomes visible even when there is some background surrounding light: first as a dull red, then yellow, and eventually a "dazzling bluish-white" as the temperature rises.[12][13] When the body appears white, it is emitting a substantial fraction of its energy asultraviolet radiation. TheSun, with aneffective temperature of approximately 5800 K,[14] is an approximate black body with an emission spectrum peaked in the central, yellow-green part of thevisible spectrum, but with significant power in the ultraviolet as well.
Blackbody radiation provides insight into thethermodynamic equilibrium state of cavity radiation.
All normal (baryonic) matter emits electromagnetic radiation when it has a temperature aboveabsolute zero. The radiation represents a conversion of a body'sinternal energy into electromagnetic energy, and is therefore calledthermal radiation. It is aspontaneous process of radiative distribution ofentropy.
Conversely, all normal matter absorbs electromagnetic radiation to some degree. An object that absorbs all radiation falling on it, at allwavelengths, is called a black body. When a black body is at a uniform temperature, its emission has a characteristic frequency distribution that depends on the temperature. Its emission is called blackbody radiation.
The concept of the black body is an idealization, as perfect black bodies do not exist in nature.[15] However,graphite andlamp black, with emissivities greater than 0.95, are good approximations to a black material. Experimentally, blackbody radiation may be established best as the ultimately stable steady state equilibrium radiation in a cavity in a rigid body, at a uniform temperature, that is entirely opaque and is only partly reflective.[15] A closed box with walls of graphite at a constant temperature with a small hole on one side produces a good approximation to ideal blackbody radiation emanating from the opening.[16][17]
Blackbody radiation has the unique absolutely stable distribution of radiative intensity that can persist in thermodynamic equilibrium in a cavity.[15] In equilibrium, for each frequency, the intensity of radiation which is emitted and reflected from a body relative to other frequencies (that is, the net amount of radiation leaving its surface, called thespectral radiance) is determined solely by the equilibrium temperature and does not depend upon the shape, material or structure of the body.[18] For a black body (a perfect absorber) there is no reflected radiation, and so the spectral radiance is entirely due to emission. In addition, a black body is a diffuse emitter (its emission is independent of direction).
Blackbody radiation becomes a visible glow of light if the temperature of the object is high enough.[19] TheDraper point is the temperature at which all solids glow a dim red, about798 K.[20] At1000 K, a small opening in the wall of a large uniformly heated opaque-walled cavity (such as an oven), viewed from outside, looks red; at6000 K, it looks white. No matter how the oven is constructed, or of what material, as long as it is built so that almost all light entering is absorbed by its walls, it will contain a good approximation to blackbody radiation. The spectrum, and therefore color, of the light that comes out will be a function of the cavity temperature alone. A graph of the spectral radiation intensity plotted versus frequency(or wavelength) is called theblackbody curve. Different curves are obtained by varying the temperature.
When the body is black, the absorption is obvious: the amount of light absorbed is all the light that hits the surface. For a black body much bigger than the wavelength, the light energy absorbed at any wavelengthλ per unit time is strictly proportional to the blackbody curve. This means that the blackbody curve is the amount of light energy emitted by a black body, which justifies the name. This is the condition for the applicability ofKirchhoff's law of thermal radiation: the blackbody curve is characteristic of thermal light, which depends only on thetemperature of the walls of the cavity, provided that the walls of the cavity are completely opaque and are not very reflective, and that the cavity is inthermodynamic equilibrium.[21] When the black body is small, so that its size is comparable to the wavelength of light, the absorption is modified, because a small object is not an efficient absorber of light of long wavelength, but the principle of strict equality of emission and absorption is always upheld in a condition of thermodynamic equilibrium.
In the laboratory, blackbody radiation is approximated by the radiation from a small hole in a large cavity, ahohlraum, in an entirely opaque body that is only partly reflective, that is maintained at a constant temperature. This technique leads to the alternative termcavity radiation. Any light entering the hole would have to reflect off the walls of the cavity multiple times before it escaped, in which process it is nearly certain to be absorbed. Absorption occurs regardless of thewavelength of the radiation entering (as long as it is small compared to the hole). The hole, then, is a close approximation of a theoretical black body and, if the cavity is heated, thespectrum of the hole's radiation (that is, the amount of light emitted from the hole at each wavelength) will be continuous, and will depend only on the temperature and the fact that the walls are opaque and at least partly absorptive, but not on the particular material of which they are built nor on the material in the cavity (compare withemission spectrum).
Theradiance or observed intensity is not a function of direction. Therefore, a black body is a perfectLambertian radiator.
Real objects never behave as full-ideal black bodies, and instead the emitted radiation at a given frequency is a fraction of what the ideal emission would be. Theemissivity of a material specifies how well a real body radiates energy as compared with a black body. This emissivity depends on factors such as temperature, emission angle, and wavelength. However, it is typical in engineering to assume that a surface's spectral emissivity and absorptivity do not depend on wavelength so that the emissivity is a constant. This is known as thegray body assumption.
With non-black surfaces, the deviations from ideal blackbody behavior are determined by both the surface structure, such as roughness or granularity, and the chemical composition. On a "per wavelength" basis, real objects in states oflocal thermodynamic equilibrium still followKirchhoff's Law: emissivity equals absorptivity, so that an object that does not absorb all incident light will also emit less radiation than an ideal black body; the incomplete absorption can be due to some of the incident light being transmitted through the body or to some of it being reflected at the surface of the body.
Inastronomy, objects such asstars are frequently regarded as black bodies, though this is often a poor approximation. An almost perfect blackbody spectrum is exhibited by thecosmic microwave background radiation.Hawking radiation is the hypothetical blackbody radiation emitted byblack holes, at a temperature that depends on the mass, charge, and spin of the hole. If this prediction is correct, black holes will very gradually shrink and evaporate over time as they lose mass by the emission of photons and other particles.
A black body radiates energy at all frequencies, but its intensity rapidly tends to zero at high frequencies (short wavelengths). For example, a black body at room temperature (300 K) with one square meter of surface area will emit a photon in the visible range (390–750 nm) at an average rate of one photon every 41 seconds, meaning that, for most practical purposes, such a black body does not emit in the visible range.[24]
The study of the laws of black bodies and the failure of classical physics to describe them helped establish the foundations ofquantum mechanics.
According to the classical theory of radiation, if eachFourier mode of the equilibrium radiation (in an otherwise empty cavity with perfectly reflective walls) is considered as a degree of freedom capable of exchanging energy, then, according to theequipartition theorem of classical physics, there would be an equal amount of energy in each mode. Since there are an infinite number of modes, this would imply infiniteheat capacity, as well as a nonphysical (i.e. not real) spectrum of emitted radiation that grows without bound with increasing frequency, predicting infinite emission power. The problem is known as theultraviolet catastrophe. Moreover, the classical theory cannot explain the experimentally observed peak in emission spectra (see alsoWien's law).
Instead, in the quantum treatment of this problem, the numbers of the energy modes arequantized, attenuating the spectrum at high frequency in agreement with experimental observation and resolving the catastrophe. The modes that had more energy than the thermal energy of the substance itself were not considered, and because of quantization modes having infinitesimally little energy were excluded.
Thus for shorter wavelengths very few modes (having energy more than) were allowed, supporting the data that the energy emitted is reduced for wavelengths less than the wavelength of the observed peak of emission.
Notice that there are two factors responsible for the shape of the graph, which can be seen as working opposite to one another. Firstly, shorter wavelengths have a larger number of modes associated with them. This accounts for the increase in spectral radiance as one moves from the longest wavelengths towards the peak at relatively shorter wavelengths. Secondly, though, at shorter wavelengths more energy is needed to reach the threshold level to occupy each mode: the more energy needed to excite the mode, the lower the probability that this mode will be occupied. As the wavelength decreases, the probability of exciting the mode becomes exceedingly small, leading to fewer of these modes being occupied: this accounts for the decrease in spectral radiance at very short wavelengths, left of the peak. Combined, they give the characteristic graph.[25]
Calculating the blackbody curve was a major challenge intheoretical physics during the late nineteenth century. The problem was solved in 1901 byMax Planck in the formalism now known asPlanck's law of blackbody radiation.[26] By making changes toWien's radiation law (not to be confused with Wien's displacement law) consistent withthermodynamics andelectromagnetism, he found a mathematical expression fitting the experimental data satisfactorily. Planck had to assume that the energy of the oscillators in the cavity was quantized, which is to say that it existed in integer multiples of some quantity.Einstein built on this idea and proposed the quantization of electromagnetic radiation itself in 1905 to explain thephotoelectric effect. These theoretical advances eventually resulted in the superseding of classical electromagnetism byquantum electrodynamics. These quanta were calledphotons and the blackbody cavity was thought of as containing agas of photons. In addition, it led to the development of quantum probability distributions, calledFermi–Dirac statistics andBose–Einstein statistics, each applicable to a different class of particles,fermions andbosons.
The wavelength at which the radiation is strongest is given by Wien's displacement law, and the overall power emitted per unit area is given by theStefan–Boltzmann law. So, as temperature increases, the glow color changes from red to yellow to white to blue. As the peak wavelength moves into the ultra-violet and further on, a tail of the spectrum will remain in the visible range and even will increase its intensity, appearing blue. It will never become invisible—indeed, the radiation of visible light increasesmonotonically with temperature.[27]
The Stefan–Boltzmann law says that the total radiant heat power emitted from a surface of a black body is proportional to the fourth power of itsabsolute temperature. The law was formulated by Josef Stefan in 1879 and later derived byLudwig Boltzmann. The formulaE =σT4 is given, whereE is the radiant heat emitted from a unit of area per unit time (power emitted from a unit area),T is the absolute temperature, andσ =5.670367×10−8 W·m−2⋅K−4 is theStefan–Boltzmann constant.[28]
Planck's law states that[29]where
For a black body surface, the spectral radiance density (defined per unit of area normal to the propagation) is independent of the angle of emission with respect to the normal. However, this means that, followingLambert's cosine law, is the radiance density per unit area of emitting surface as the surface area involved in generating the radiance is increased by a factor with respect to an area normal to the propagation direction. At oblique angles, the solid angle spans involved do get smaller, resulting in lower aggregate intensities.
The emitted energy flux density or irradiance, is related to the photon flux density through[30]
Wien's displacement law shows how the spectrum of blackbody radiation at any temperature is related to the spectrum at any other temperature. If we know the shape of the spectrum at one temperature, we can calculate the shape at any other temperature. Spectral intensity can be expressed as a function of wavelength or of frequency.
A consequence of Wien's displacement law is that the wavelength at which the intensityper unit wavelength of the radiation produced by a black body has a local maximum or peak,, is a function only of the temperature:where the constantb, known as Wien's displacement constant, is equal to[31]and is theLambert W function. At a typical room temperature of 293 K (20 °C), the maximum intensity is at9.9 μm.
Planck's law was also stated above as a function of frequency. The intensity maximum for this is given by[32]In unitless form, the maximum occurs when, where. The approximate numerical solution is. At a typical room temperature of 293 K (20 °C), the maximum intensity is for = 17 THz.
By integrating over the frequency the radiance (units: power / [area × solid angle] ) isby using with and with being theStefan–Boltzmann constant.
On a side note, at a distance d, the intensity per area of radiating surface is the useful expressionwhen the receiving surface is perpendicular to the radiation.
By subsequently integrating over the solid angle for all azimuthal angle (0 to) and polar angle from 0 to, we arrive at theStefan–Boltzmann law: the powerj* emitted per unit area of the surface of a black body is directly proportional to the fourth power of its absolute temperature:We used
The human body radiates energy asinfrared light. The net power radiated is the difference between the power emitted and the power absorbed:Applying the Stefan–Boltzmann law,whereA andT are the body surface area and temperature, is theemissivity, andT0 is the ambient temperature.
The total surface area of an adult is about2 m2, and the mid- and far-infraredemissivity of skin and most clothing is near unity, as it is for most nonmetallic surfaces.[33][34] Skin temperature is about 33 °C,[35] but clothing reduces the surface temperature to about 28 °C when the ambient temperature is 20 °C.[36] Hence, the net radiative heat loss is aboutThe total energy radiated in one day is about 8MJ, or 2000 kcal (foodcalories).Basal metabolic rate for a 40-year-old male is about 35 kcal/(m2·h),[37] which is equivalent to 1700 kcal per day, assuming the same 2 m2 area. However, the mean metabolic rate of sedentary adults is about 50% to 70% greater than their basal rate.[38]
There are other important thermal loss mechanisms, includingconvection andevaporation. Conduction is negligible – theNusselt number is much greater than unity. Evaporation byperspiration is only required if radiation and convection are insufficient to maintain a steady-state temperature (but evaporation from the lungs occurs regardless). Free-convection rates are comparable, albeit somewhat lower, than radiative rates.[39] Thus, radiation accounts for about two-thirds of thermal energy loss in cool, still air. Given the approximate nature of many of the assumptions, this can only be taken as a crude estimate. Ambient air motion, causing forced convection, or evaporation reduces the relative importance of radiation as a thermal-loss mechanism.
Application ofWien's law to human-body emission results in a peak wavelength ofFor this reason, thermal imaging devices for human subjects are most sensitive in the 7–14 micrometer range.
The blackbody law may be used to estimate the temperature of a planet orbiting the Sun.
The temperature of a planet depends on several factors:
The analysis only considers the Sun's heat for a planet in aSolar System.
TheStefan–Boltzmann law gives the totalpower (energy/second) that the Sun emits:
| 1 |
where
The Sun emits that power equally in all directions. Because of this, the planet is hit with only a tiny fraction of it. The power from the Sun that strikes the planet (at the top of the atmosphere) is:
| 2 |
where
Because of its high temperature, the Sun emits to a large extent in the ultraviolet and visible (UV-Vis) frequency range. In this frequency range, the planet reflects a fraction of this energy where is thealbedo or reflectance of the planet in the UV-Vis range. In other words, the planet absorbs a fraction of the Sun's light, and reflects the rest. The power absorbed by the planet and its atmosphere is then:
| 3 |
Even though the planet only absorbs as a circular area, it emits in all directions; the spherical surface area being. If the planet were a perfect black body, it would emit according to theStefan–Boltzmann law
| 4 |
where is the temperature of the planet. This temperature, calculated for the case of the planet acting as a black body by setting, is known as theeffective temperature. The actual temperature of the planet will likely be different, depending on its surface and atmospheric properties. Ignoring the atmosphere and greenhouse effect, the planet, since it is at a much lower temperature than the Sun, emits mostly in the infrared (IR) portion of the spectrum. In this frequency range, it emits of the radiation that a black body would emit where is the average emissivity in the IR range. The power emitted by the planet is then:
| 5 |
For a body inradiative exchange equilibrium with its surroundings, the rate at which it emitsradiant energy is equal to the rate at which it absorbs it:[40][41]
| 6 |
Substituting the expressions for solar and planet power in equations 1–6 and simplifying yields the estimated temperature of the planet, ignoring greenhouse effect,TP:
| 7 |
In other words, given the assumptions made, the temperature of a planet depends only on the surface temperature of the Sun, the radius of the Sun, the distance between the planet and the Sun, the albedo and the IR emissivity of the planet.
Notice that a gray (flat spectrum) ball where comes to the same temperature as a black body no matter how dark or light gray.
Substituting the measured values for the Sun and Earth yields:
With the average emissivity set to unity, theeffective temperature of the Earth is:or −18.8 °C.
This is the temperature of the Earth if it radiated as a perfect black body in the infrared, assuming an unchanging albedo and ignoringgreenhouse effects (which can raise the surface temperature of a body above what it would be if it were a perfect black body in all spectrums[44]). The Earth in fact radiates not quite as a perfect black body in the infrared which will raise the estimated temperature a few degrees above the effective temperature. If we wish to estimate what the temperature of the Earth would be if it had no atmosphere, then we could take the albedo and emissivity of the Moon as a good estimate. The albedo and emissivity of the Moon are about 0.1054[45] and 0.95[46] respectively, yielding an estimated temperature of about 1.36 °C.
Estimates of the Earth's average albedo vary in the range 0.3–0.4, resulting in different estimated effective temperatures. Estimates are often based on thesolar constant (total insolation power density) rather than the temperature, size, and distance of the Sun. For example, using 0.4 for albedo, and an insolation of 1400 W m−2, one obtains an effective temperature of about 245 K.[47]Similarly using albedo 0.3 and solar constant of 1372 W m−2, one obtains an effective temperature of 255 K.[48][49][50]
Thecosmic microwave background radiation observed today is the most perfect blackbody radiation ever observed in nature, with a temperature of about 2.7 K.[51] It is a "snapshot" of the radiation at the time ofdecoupling between matter and radiation in the early universe. Prior to this time, most matter in the universe was in the form of an ionized plasma in thermal, though not full thermodynamic, equilibrium with radiation.
At very high temperatures (above 1010 K; such temperatures existed in the very early universe), where the thermal motion separates protons and neutrons in spite of the strong nuclear forces, electron-positron pairs appear and disappear spontaneously and are in thermal equilibrium with electromagnetic radiation. These particles form a part of the black body spectrum, in addition to the electromagnetic radiation.[52]
A black body at room temperature (23 °C (296 K; 73 °F)) radiates mostly in theinfrared spectrum, which cannot be perceived by the human eye,[53] but can be sensed by some reptiles. As the object increases in temperature to about 500 °C (773 K; 932 °F), the emission spectrum gets stronger and extends into the human visual range, and the object appears dull red. As its temperature increases further, it emits more and more orange, yellow, green, and then blue light (and ultimately beyond violet,ultraviolet).
Tungsten filament lights have a continuous black body spectrum with a colour temperature of around 2,700 K (2,430 °C; 4,400 °F), and also emits considerable energy in the infrared range. Modern-dayfluorescent andLED lights, which are more efficient, do not have a continuous black body emission spectrum, rather emitting directly, or using combinations of phosphors that emit multiple narrow spectrums.
In query 6 ofIsaac Newton'sOpticks, he states that "Do not black Bodies conceive heat more easily from Light than those of other Colours do, by reason that the Light falling on them is not reflected outwards, but enters into the Bodies, and is often reflected and refracted within them, until it be stifled and lost?", thereby introducing the notion of ablack body.[54][55][56] In his first memoir,Augustin-Jean Fresnel (1788–1827) responded to a view he extracted from a French translation of Newton'sOpticks. He says that Newton imagined particles of light traversing space uninhibited by thecaloric medium filling it, and refutes this view (never actually held by Newton) by saying that a black body under illumination would increase indefinitely in heat.[57]
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.[58] Stewart chose lamp-black surfaces as his reference because of various previous experimental findings, especially those ofPierre Prevost and ofJohn 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's statement assumed a general principle: that there exists a body or surface that has the greatest possible absorbing and radiative power for every wavelength and equilibrium temperature.
Stewart was concerned with selective thermal radiation, which he investigated using plates which selectively radiated and absorbed different wavelengths. He discussed the experiments in terms of rays which could be reflected and refracted, and which obeyed the Stokes-Helmholtz reciprocity principle. His research did not consider that properties of rays are dependent on wavelength, and he did not use tools 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.
In 1859,Gustav Robert Kirchhoff reported the coincidence of the wavelengths of spectrally resolved lines of absorption and 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.[59]
Kirchhoff then went on to consider some bodies that emit and absorb heat radiation, in an opaque enclosure or cavity, in equilibrium at a temperatureT.
Here is used a notation different from Kirchhoff's. Here, the emitting powerE(T,i) denotes a dimensioned quantity, the total radiation emitted by a body labeled by indexi at temperatureT. The total absorption ratioa(T,i) of that body is dimensionless, the ratio of absorbed to incident radiation in the cavity at temperatureT . (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 ratioE(T,i) /a(T,i) of emitting power to absorptivity is a dimensioned quantity, with the dimensions of emitting power, becausea(T,i) is dimensionless. Also here the wavelength-specific emitting power of the body at temperatureT is denoted byE(λ,T,i) and the wavelength-specific absorption ratio bya(λ,T,i) . Again, the ratioE(λ,T,i) /a(λ,T,i) of emitting power to absorptivity 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.[60] His theoretical proof was and still is considered by some writers to be invalid.[61][62] 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 absorptivity 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 ratioE(λ,T,i) /a(λ,T,i) has one and the same value for all bodies. 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 emitted and absorbed by a body in equilibrium, the dimensioned total radiation ratioE(T,i) /a(T,i) has one and the same value common to all bodies.[63] 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 ratioE(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.[61][62]
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.[64]
Kirchhoff's proof considered an arbitrary non-ideal body labeledi as well as various perfect black bodies labeledBB. It required that the bodies be kept in a cavity in thermal equilibrium at temperatureT. His proof intended to show that the ratioE(λ,T,i) /a(λ,T,i) was independent of the naturei of the non-ideal body, however partly transparent or partly reflective it was.
His proof first argued that for wavelengthλ and at temperatureT, at thermal equilibrium, all perfectly black bodies of the same size and shape have the one and the same common value of emissive powerE(λ,T, BB), with the dimensions of power. His proof noted that the dimensionless wavelength-specific absorptivitya(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 absorptivityE(λ,T, BB) /a(λ,T, BB) is again justE(λ,T, BB), with the dimensions of power. Kirchhoff considered 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 temperatureT. He argued that the flows of heat radiation must be the same in each case. Thus he argued that at thermal equilibrium the ratioE(λ,T,i) /a(λ,T,i) was equal toE(λ,T, BB), which may now be denotedBλ (λ,T).Bλ (λ,T) is a continuous function, dependent only onλ at fixed temperatureT, and an increasing function ofT at fixed wavelengthλ. It vanishes at low temperatures for visible wavelengths, which does not depend on the naturei of the arbitrary non-ideal body (Geometrical factors, taken into detailed account by Kirchhoff, have been ignored in the foregoing).
ThusKirchhoff's law of thermal radiation can be stated:For any material at all, radiating and absorbing in thermodynamic equilibrium at any given temperatureT, for every wavelengthλ, the ratio of emissive power to absorptivity has one universal value, which is characteristic of a perfect black body, and is an emissive power which we here represent byBλ (λ, T). (For our notationBλ (λ,T), Kirchhoff's original notation was simplye.)[63][65][66][67][68][69]
Kirchhoff announced that the determination of the functionBλ (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. Occasionally by historians that functionBλ (λ,T) has been called "Kirchhoff's (emission, universal) function,"[70][71][72][73] 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.[62] Kirchhoff stated later in 1860 that his theoretical proof was better than Balfour Stewart's, and in some respects it was so.[61] 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 withCarnot's principle, which is a form of the second law.[74]
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."[75]
Therelativistic Doppler effect causes a shift in the frequencyf of light originating from a source that is moving in relation to the observer, so that the wave is observed to have frequencyf':wherev is the velocity of the source in the observer's rest frame,θ is the angle between the velocity vector and the observer-source direction measured in the reference frame of the source, andc is thespeed of light.[76] This can be simplified for the special cases of objects moving directly towards (θ = π) or away (θ = 0) from the observer, and for speeds much less thanc.
Through Planck's law the temperature spectrum of a black body is proportionally related to the frequency of light and one may substitute the temperature (T) for the frequency in this equation.
For the case of a source moving directly towards or away from the observer, this reduces toHerev > 0 indicates a receding source, andv < 0 indicates an approaching source.
This is an important effect in astronomy, where the velocities of stars and galaxies can reach significant fractions ofc. An example is found in thecosmic microwave background radiation, which exhibits a dipole anisotropy from the Earth's motion relative to this blackbody radiation field.
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