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Black Body Radiation

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Black Body Radiation

A black body (or blackbody) is a term used in physics to refer to an object that absorbs all incoming energy, no matter its frequency. Black bodies have no reflective power, so no radiation is reflected, and the object appears black to the eye. Black bodies can also emit radiation (called black body radiation), which is done perfectly (without internal dissipation). When black bodies are in equilibrium, there is a relationship between their temperature and their emission properties, which was first studied by the scientist Gustav Kirchhoff.

The reason behind perfect absorbers being perfect emitters is because the processes are the inverse of each other. In the case of electromagnetic energy, the absorption and emission process involves the absorption and emission of photons.

The definition of black body radiation

When a black body is in equilibrium, the amount of energy entering a region of the object equals the energy leaving the same region. The radiation emitted by a black body is known as black body radiation, which has a continuous spectrum known as the black body spectrum, whose pattern is very well known (see the image below for examples).

Why does classical mechanics fail to explain the black body spectrum?

Classical mechanics fails to explain this spectrum because, according to the models, particles could vibrate at higher energies without any limit with increasing intensity. This would produce a spectrum with increasing values of intensity at higher frequencies (larger vibrations). However, the intensities in the black body spectrum are known to decrease with the wavelength approaching zero, which you can see in the image below. In the image, the curves in red, green, and blue correspond to different temperatures. The peaks of the emission intensity correspond to different frequencies that depend on the temperature.

Black body radiation Black body spectrum StudySmarterBlack body spectrum, Wikimedia Commons

It was not until the end of the nineteenth century that German-born scientist Max Planck came up with an idea to solve the disagreement between theory and experiments. In Planck’s model, energy was not shared between particles on arbitrary continuous values: it was only shared in fixed amounts that were multiples of a number “h”.

In light, for very high frequencies, the kinetic energy is calculated as h·f (where f is the frequency). It cannot be translated into thermal energy at these frequencies because this would mean infinite temperatures. This means that the constituents of the black body gradually plunge towards the region where they have no temperature, which you can see in the left part of the above image.

The right part of the image was perfectly understood without quantum physics because, for very low frequencies, the equivalent thermal energy is also very low. The understanding of the regime of high frequencies led to the prediction of the existence of photons, which were carrying the "quanta" (discrete pieces of energy measured by the constant h).

Characteristics of the black body spectrum

The most intensely emitted radiation by an object has a wavelength λ that is inversely proportional to the temperature. Higher temperatures will emit intense radiation at shorter wavelengths, and the colour will shift to the blue spectrum. The spectrum of radiation has the following characteristics:

  • The spectrum is continuous.

  • The spectrum peak moves to shorter wavelengths as the temperature increases.

  • The spectrum is 0 at 0 – this is the result of the quantisation of energy.

  • The spectrum values at larger wavelengths are smaller.

Astronomical objects can be modelled as black bodies. This is why black body radiation is very useful in physics, astrophysics, and astronomy.

Black body radiation colour chart

Temperature, wavelength emission, and colour perceived are related quantities for a black body. A colour chart can show the temperature-colour dependence of a black body. In astronomy, we can approximate the temperatures of astronomical objects by characterising their emission properties, as shown in the image below.

Black body radiation Black body diagram in sRGB StudySmarterBlack body diagram in sRBG from 1000K to 10,000K, Wikimedia Commons

The colours observed for any object are the product of the light (photons) emitted by the object or reflected by the object. Photons have a different wavelength depending on their energy: low energy photons are perceived as red, and high energy photons are perceived as blue-violet.

The colour difference you perceive is due to cells known as cone cells. Cone cells are very special photoreceptor cells that can convert incident light into an electrical signal that is delivered to the brain.

Cone cells are divided into three types of cells that are sensitive to a range of different wavelengths: short wavelengths like blue and purple colours, medium wavelengths like green and yellow, and large wavelengths like orange and red.

Stars and black body radiation

Stars can be modelled as black bodies, meaning their surface temperature and wavelength emission are related. Thanks to this relationship, we can differentiate which stars have a higher temperature than others by the radiation they emit and the observed colour. See the table below for some examples (where K stands for Kelvin and nm for nanometers):

ColourStar nameTemperature (K)Peak emission (nm)
Blue-WhiteRigel11,000145
Blue-WhiteVega9602310
YellowSun5778550
OrangeAldebaran3910740

Stars do not exhibit the same colour throughout their lifetimes, and the colour variation can tell us a lot about the temperature and processes happening inside.

One example is the specific case of a yellow star, like our Sun, that will become a red giant.

A star exists thanks to a process of nuclear fusion that happens inside it. This process primarily fuses hydrogen and helium, creating heavier elements. During fusion, the core of a star is in equilibrium, gravity tries to compress it, and fusion tries to expand it.

Black body radiation Balances of forces in a star StudySmarterThe balance of forces in a star dictates its size, colour, and emission in the case of stars that become red giants. Manuel R. Camacho – StudySmarter Originals

As the hydrogen is exhausted, the star’s core starts to compress due to gravity as the force balance is broken and the compression heats the nucleus. As a result, the star’s outer layers heat up, and the fusion process happens in the outer layers.

Black body radiation Balances of forces in a star StudySmarterWhen the balance of forces in a star is broken, as in the case of red giants, the upper layers increase their size, and the surface lowers its temperature becoming reddish. Manuel R. Camacho – StudySmarter Originals

The process expands the star’s outer surface, and the surface cools down. During this process, the star becomes a red giant. As a result, the star’s colour goes from yellow to red, and its emission shifts to larger wavelengths (lower surface temperatures).

If you go outside during the night in some parts of the Northern Hemisphere and there is a clear sky, you may be able to see two stars: Betelgeuse and Rigel.

In the image below, the upper left red star is Betelgeuse. This star is a red supergiant star, and, as such, it must have a peak emission on the red spectrum. The star below Betelgeuse to the right is Rigel, and its blue colour indicates that its spectral peak must be around a blue-purple.

Black body radiation Position of Betelgeuse and Rigel in the constellation of Orion StudySmarterPosition of Betelgeuse and Rigel in Orion, Wikimedia Commons

The emission peak of Rigel is measured at around 145nm. Meanwhile, the emission peak of Betelgeuse is measured at around 855nm. If you look at the table of colour spectra, you can see that the colour of Betelgeuse corresponds to a larger wavelength (red colours) and Rigel to a shorter wavelength (purple-blue colours).

Due to the law that connects the energy of photons with the frequency, we know that the photons emitted by Rigel have more energy than the photons emitted by Betelgeuse.

Application of black body radiation to black holes

Black holes are astronomical objects that can be modelled as black bodies. In this case, black holes are modelled as perfect absorbers that do not let any radiation escape. Black holes are still under heavy research, but they are expected to emit some kind of radiation as perfect absorbers.

A suggested mechanism proposed by the British scientist Stephen Hawking – known as Hawking radiation – takes the form of a black body radiation curve. However, no definitive answers have been found for these phenomena.

Black Body Radiation - Key takeaways

  • A black body is a perfect emitter and absorber of radiation. In a black body, the radiation emission depends on its temperature.
  • Because of the temperature-emission-frequency relationship, the emission peak gives us the body’s temperature.
  • Stars, as emitting bodies, can be modelled as black bodies. Because of this, the colour of the star can tell us about its temperature. Red stars will be colder and blue stars will be hotter.
  • Black holes are perfect black bodies, able to absorb all radiation. Several mechanisms have been predicted and theorised by which they can emit radiation. One of them is the Hawking radiation.

Frequently Asked Questions about Black Body Radiation

Black body radiation is the radiation emitted by a perfect absorber and emitter (a black body).

Classical theory predicted that the intensity of emission would increase as frequencies became higher. However, it did not take into account quantum effects that become relevant at very high frequencies and lead to a drop in the intensity of emission.

As the explanation given by Max Planck required light (radiation) to have discrete values, the light had to be emitted in small packages or particles known as photons. This is how black body radiation proves the particle nature of light.

When a black body is in equilibrium, the amount of energy entering a region of the object equals the energy leaving the same region. The radiation emitted by a black body is known as black body radiation, which has a continuous spectrum known as the black body spectrum, whose pattern is very well known.

Black body radiation was predicted by Gustav R. Kirchhoff. However, it was Max Planck who was able to describe the behaviour of black body radiation.

Final Black Body Radiation Quiz

Question

What is a black body?

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Answer

An object that cannot reflect energy.

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Question

What is black body radiation?

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Answer

The radiation emitted from a black body.

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Question

Name the scientist who described black body radiation.

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Answer

Gustav R. Kirchhoff.

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Question

Name the scientist who solved the inconsistencies of black body radiation with classical mechanics.

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Answer

Max Planck. 

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Question

For black body radiation, does the colour depend on the temperature? 

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Answer

Yes.

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Question

Is a red emitter warmer than a blue emitter? 


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Answer

No, because blue corresponds to a light spectrum with higher frequencies, hence higher energies.

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Question

Stars can be modelled as blackbodies? True or false?


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Answer

True.

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Question

What is the average temperature of the Sun’s surface?

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Answer

5778K

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Question

Is a blue star colder than our Sun? 

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Answer

No, blue stars have a higher frequency emission, hence they are hotter.

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Question

Betelgeuse’s surface is warmer than the Sun. True or false?

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Answer

False, Betelgeuse’s surface is colder than the Sun.

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Question

Can black holes be modelled as black bodies?

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Answer

Yes, as they are near-perfect absorbers.

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Question

Why are perfect emitters also good absorbers?

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Answer

Because the processes of emission and absorption are the inverse of each other.

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Question

Which star surface is warmer? Vega, whose colour is near white, or the Sun, whose colour is yellow?

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Answer

Vega has a warmer surface. 

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Question

Give the equation that describes the quantisation of energy.

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Answer

E=n⋅h⋅f

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