Black body

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WMAP image of the cosmic microwave background radiation anisotropy. It has the most perfect thermal emission spectrum known and corresponds to a temperature of 2.725 Kelvin with an emission peak at 160.4 GHz.

In physics, a black body is an object that absorbs all electromagnetic radiation that falls onto it. No radiation passes through it and none is reflected. It is this lack of both transmission and reflection to which the name refers. These properties make black bodies ideal sources of purely thermal radiation. That is, the amount and wavelength (color) of electromagnetic radiation they emit is directly related to their temperature. Black bodies below around 700 K (430 °C) produce very little radiation at visible wavelengths and appear black (hence the name). Black bodies above this temperature, however, begin to produce radiation at visible wavelengths starting at red, going through orange, yellow, and white before ending up at blue as the temperature increases.

The term "black body" was introduced by Gustav Kirchhoff in 1860. The light emitted by a black body is called black-body radiation, and has a special place in the History of quantum mechanics.^[1]

1 Explanation
2 Equations governing black bodies
3 Radiation emitted by a human
4 Temperature relation between a planet and its star
5 Historical examples of black body radiation
6 See also
7 References
- 7.1 Other textbooks
8 External links

[edit] Explanation

As the temperature decreases, the peak of the black body radiation curve moves to lower intensities and longer wavelengths. The black-body radiation graph is also compared with the classical model of Rayleigh and Jeans.

In the laboratory, the closest thing to black-body radiation is the radiation from a small hole entrance to a larger cavity. 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. This occurs regardless of the wavelength 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, the spectrum of the hole's radiation (i.e., the amount of light emitted from the hole at each wavelength) will be continuous, and will not depend on the material in the cavity (compare with emission spectrum). By a theorem proved by Kirchhoff, this curve depends only on the temperature of the cavity walls. ^[2]

Calculating this curve was a major challenge in theoretical physics during the late nineteenth century. The problem was finally solved in 1901 by Max Planck as Planck's law of black-body radiation ^[3] . By making changes to Wien's Radiation Law (not to be confused with Wien's displacement law) consistent with Thermodynamics and Electromagnetism, he found a mathematical formula fitting the experimental data in a satisfactory way. To find a physical interpretation for this formula, Planck had then to assume that the energy of the oscillators in the cavity was quantized (i.e., integer multiples of some quantity). Einstein built on this idea and proposed the quantization of electromagnetic radiation itself in 1905 to explain the photoelectric effect. These theoretical advances eventually resulted in the superseding of classical electromagnetism by quantum electrodynamics. Today, these quanta are called photons and the black body cavity may be thought of as containing a gas of photons. In addition, it led to the development of quantum versions of statistical mechanics, called Fermi-Dirac statistics and Bose-Einstein statistics, each applicable to a different class of particles. See also fermion and boson.

The temperature of a Pahoehoe lava flow can be estimated by observing its colour. The result agrees nicely with the measured temperatures of lava flows at about 1,000 to 1,200 °C.

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 the Stefan-Boltzmann law. So, as temperature increases, the glow color changes from red to yellow to white to blue. Even as the peak wavelength moves into the ultra-violet enough radiation continues to be emitted in the blue wavelengths that the body will continue to appear blue. It will never become invisible—indeed, the radiation of visible light increases monotonically with temperature.^[4]

The radiance or observed intensity is not a function of direction. Therefore a black body is a perfect Lambertian 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. The emissivity 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 the grey body assumption.

Although Planck's formula predicts that a black body will radiate energy at all frequencies, the formula is only applicable when many photons are being measured. For example, a black body at room temperature (300 kelvin) with one square meter of surface area will emit a photon in the visible range once every thousand years or so, meaning that for most practical purposes, the black body does not emit in the visible range.

When dealing with non-black surfaces, the deviations from ideal black body behavior are determined by both the geometrical structure and the chemical composition, and follow Kirchhoff'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.

In astronomy, objects such as stars are frequently regarded as black bodies, though this is often a poor approximation. An almost perfect black-body spectrum is exhibited by the cosmic microwave background radiation. Hawking radiation is black-body radiation emitted by black holes.

[edit] Equations governing black bodies

[edit] Planck's law of black-body radiation

Main article: Planck's law of black-body radiation

$I(\nu) = \frac{2 h\nu^{3}}{c^2}\frac{1}{e^{\frac{h\nu}{kT}}-1}$

where

$I(\nu)d\nu \,$ is the amount of energy per unit surface per unit time per unit solid angle emitted in the frequency range between ν and ν+dν;
$T \,$ is the temperature of the black body;
$h \,$ is Planck's constant;
$c \,$ is the speed of light; and
$k \,$ is Boltzmann's constant.

[edit] Wien's displacement law

Main article: Wien's displacement law

The relationship between the temperature T of a black body, and wavelength $λ m a x$ at which the intensity of the radiation it produces is at a maximum is

$T \lambda_\mathrm{max} = 2.898... \times 10^6 \ \mathrm{nm \ K}. \,$

The nanometer is a convenient unit of measure for optical wavelengths. Note that 1 nanometer is equivalent to 10⁻⁹ meters.

[edit] Stefan-Boltzmann law

Main article: Stefan-Boltzmann law

The total energy radiated per unit area per unit time $j^{\star}$ (in watts per square meter) by a black body is related to its temperature T (in kelvins) and the Stefan-Boltzmann constant $σ$ as follows:

$j^{\star} = \sigma T^4.\,$

[edit] Radiation emitted by a human

Much of a person's energy is radiated away in the form of infrared energy.

Black-body laws can be applied to many things. For example, a great deal of a person's energy is radiated away in the form of electromagnetic radiation - of which, most is infrared.

The net power (energy/second) of energy radiated away is the difference between what someone absorbs from their surroundings and what they radiate themselves:

$P_{net}=P_{emit}-P_{absorb} \,$

Plugging in the Stefan-Boltzmann law:

$P_{net}=A\sigma \epsilon \left( T^4 - T_{0}^4 \right) \,$

The above equation is applicable to any object which behaves similar to a black body. People have an area of about 2 square meters, and emissivity of nearly 1. They also have a skin temperature of about 32 °C (90 °F, or 305 K). But clothing reduces the surface temperature a few degrees, so in addition to reducing heat loss through conduction, it reduces loss of heat by radiation. So for surface temperature of people we should use 301 K. The temperature of the surrounding environment varies, but for a rough order of magnitude answer, one can use 20 °C (68 °F, or 293 K). Plugging in these values results in a net rate emission of energy for people of about:

$P_{net} = 95 \ \mathrm{watts} \,$

In this scenario, people are roughly 100 watt light bulbs, except they emit all infrared and longer wavelength light. The amount of energy in a whole day turns out to be almost 9 million joules, or 2,000 (food) calories. Normal rate of metabolism is typically 100-120 watts, and a person losing more than 160 watts (with extra losses by evaporation, convection and conduction) would feel cold and need to increase activity or cover with clothes. In contrast, during physical activity the metabolism is much higher and since the emission is not large enough, the excess heat is carried by sweating.

Also, applying Wien's Law to humans, one finds that the peak wavelength of light emitted by a person is:

$\lambda_{peak} = \frac{2.898\times 10^6 \ \mathrm{K} \cdot \mathrm{nm}}{305 \ \mathrm{K}} = 9500 \ \mathrm{nm} \,$

This, presumably, would be the wavelength that infrared goggles would be designed to be most sensitive to. (In fact, 7-14 micrometers is a typical spectral response range for thermal imaging devices designed for human subjects.)

[edit] Temperature relation between a planet and its star

Here is an application of black-body laws. It is a rough derivation that gives an order of magnitude answer. See p. 380-382 of Planetary Science, for further discussion.^[5]

[edit] Assumptions

The surface temperature of a planet depends on a few factors:

Incident radiation (from the sun, for example)
The albedo effect (the fraction of light a planet reflects)
The greenhouse effect (for planets with an atmosphere)
Energy generated internally by a planet itself (This is more important for planets like Jupiter)

For the inner planets, incident radiation has the most significant impact on surface temperature. This derivation is concerned mainly with that.

If we assume the following:

The Sun and the Earth both radiate as spherical black bodies in thermal equilibrium with themselves.
The Earth absorbs all the solar energy that it intercepts from the Sun.

then we can derive a formula for the relationship between the Earth's surface temperature and the Sun's surface temperature.

[edit] Derivation

To begin, we use the Stefan-Boltzmann law to find the total power (energy/second) the Sun is emitting:

The Earth only has an absorbing area equal to a two dimensional circle, rather than the surface of a sphere.

$P_{S emt} = \left( \sigma T_{S}^4 \right) \left( 4 \pi R_{S}^2 \right) \qquad \qquad (1)$

where

$\sigma \,$ is the Stefan-boltzmann constant,

$T_S \,$ is the surface temperature of the Sun, and

$R_S \,$ is the radius of the Sun.

The Sun emits that power equally in all directions. Because of this, the Earth is hit with only a tiny fraction of it. This is the power from the Sun that the Earth absorbs:

$P_{E abs} = P_{S emt} \left( \frac{\pi R_{E}^2}{4 \pi D^2} \right) \qquad \qquad (2)$

where

$R_{E} \,$ is the radius of the Earth and

$D \,$ is the distance between the Sun and the Earth.

Even though the earth only absorbs as a circular area $π R 2$ , it emits equally in all directions as a sphere:

$P_{E emt} = \left( \sigma T_{E}^4 \right) \left( 4 \pi R_{E}^2 \right) \qquad \qquad (3)$

where

T E

is the surface temperature of the earth.

Now, in the first assumption the earth is in thermal equilibrium, so the power absorbed must equal the power emitted:

$P_{E abs} = P_{E emt}\,$

So plug in equations 1, 2, and 3 into this and we get

$\left( \sigma T_{S}^4 \right) \left( 4 \pi R_{S}^2 \right) \left( \frac{\pi R_{E}^2}{4 \pi D^2} \right) = \left( \sigma T_{E}^4 \right) \left( 4 \pi R_{E}^2 \right).\,$

Many factors cancel from both sides and this equation can be greatly simplified.

[edit] The result

After canceling of factors, the final result is

$T_{S}\sqrt{\frac{R_{S}}{2 D}} = T_{E}$

where

$T_S \,$ is the surface temperature of the Sun,

$R_S \,$ is the radius of the Sun,

$D \,$ is the distance between the Sun and the Earth, and

$T_E \,$ is the average surface temperature of the Earth.

In other words, the temperature of the Earth only depends on the surface temperature of the Sun, the radius of the Sun, and the distance between the Earth and the Sun.

[edit] Temperature of the Sun

If we substitute in the measured values for Earth,

$T_{E} \approx 14 \ \mathrm{{}^\circ C} = 287 \ \mathrm{K},$

$R_{S} = 6.96 \times 10^8 \ \mathrm{m},$

$D = 1.5 \times 10^{11} \ \mathrm{m},$

we'll find the surface temperature of the Sun to be

$T_{S} \approx 5960 \ \mathrm{K}.$

This is within three percent of the standard measure of 5780 kelvins which makes the formula valid for most scientific and engineering applications.

[edit] Historical examples of black body radiation

Blast furnaces before 1700 heated with charcoal could only produce "red hot" pig iron. The introduction of coke for heating in English ironworks in 1709 enabled "yellow hot" iron, required for the more advanced products of the Industrial Revolution.

[edit] See also

[edit] References

^ When used as a compound adjective, the term is typically hyphenated, as in "black-body radiation", or combined into one word, as in "blackbody radiation". The hyphenated and one-word forms should not generally be used as nouns, however.
^ Huang, Kerson (1967). Statistical Mechanics. New York: John Wiley & Sons.
^ Planck, Max (1901). "On the Law of Distribution of Energy in the Normal Spectrum" (HTML). Annalen der Physik 4: 553.
^ Landau, L. D.; E. M. Lifshitz (1996). Statistical Physics, 3rd Edition Part 1, Oxford: Butterworth-Heinemann.
^ Cole, George H. A.; Woolfson, Michael M. (2002). Planetary Science: The Science of Planets Around Stars (1st ed.). Institute of Physics Publishing. ISBN 0-7503-0815-X.

[edit] Other textbooks

Kroemer, Herbert; Kittel, Charles (1980). Thermal Physics (2nd ed.). W. H. Freeman Company. ISBN 0-7167-1088-9.
Tipler, Paul; Llewellyn, Ralph (2002). Modern Physics (4th ed.). W. H. Freeman. ISBN 0-7167-4345-0.

[edit] External links

Interactive Blackbody Radiance Calculator - Includes all common units and an in-depth description of formulas.
Cooling Mechanisms for Human Body - From Hyperphysics
Descriptions of radiation emitted by many different objects
Black Body Emission Calculator
Black Body Emission Applet

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Categories: Thermodynamics | Electromagnetic radiation | Astrophysics

Black body

From Wikipedia, the free encyclopedia

Contents

[edit] Explanation

[edit] Equations governing black bodies

[edit] Planck's law of black-body radiation

[edit] Wien's displacement law

[edit] Stefan-Boltzmann law

[edit] Radiation emitted by a human

[edit] Temperature relation between a planet and its star

[edit] Assumptions

[edit] Derivation

[edit] The result

[edit] Temperature of the Sun

[edit] Historical examples of black body radiation

[edit] See also

[edit] References

[edit] Other textbooks

[edit] External links

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