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Wiens Law: Difference between revisions

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[[File:Wien_Displacement.png|400px|framed|right|Figure 1. Blackbody radiation curves for a blackbody at four different temperatures, displaying the shift in peak wavelength for two different temperatures.<ref>"Wien Displacement" Licensed under CC BY-SA 3.0 via Wikimedia Commons - http://commons.wikimedia.org/wiki/File:Wien_Displacement.png#/media/File:Wien_Displacement.png</ref>]]
[[File:Wien_Displacement.png|400px|framed|right|Figure 1. Blackbody radiation curves for a blackbody at four different temperatures, displaying the shift in peak wavelength for two different temperatures.<ref>"Wien Displacement" Licensed under CC BY-SA 3.0 via Wikimedia Commons - http://commons.wikimedia.org/wiki/File:Wien_Displacement.png#/media/File:Wien_Displacement.png</ref>]]
<onlyinclude>'''Wien's Law''', sometimes called ''Wien's Displacement Law'', is a law that determines at what [[wavelength]] the intensity of [[radiation]] emitted from a [[blackbody radiation|blackbody]] reaches its maximum point.</onlyinclude><ref name='krane'>Kenneth Krane. Modern Physics, 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.</ref> After this point, the intensity decreases as [[temperature]] increases. This creates the characteristic shape of blackbody radiation curves. Wien's Law is expressed simply as:<ref>Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003.</ref>
<onlyinclude>'''Wien's Law''', sometimes called ''Wien's Displacement Law'', is a law that determines at what [[wavelength]] the intensity of [[radiation]] emitted from a [[blackbody radiation|blackbody]] reaches its maximum point.</onlyinclude><ref name='krane'>Kenneth Krane. Modern Physics, 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.</ref> After this point, the intensity decreases as [[temperature]] increases. This creates the characteristic shape of blackbody radiation curves. Wien's Law is expressed simply as:<ref>Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003.</ref>


<center><math> \lambda_{max} \times T = 2.8978 \times 10^{-3} mK </math></center>
<center><math> \lambda_{max} \times T = 2.8978 \times 10^{-3} \textrm{m}\cdot\textrm{K} </math></center>


Where <math>\lambda</math> is the wavelength in [[meter]]s, and <math>T</math> is the temperature in [[Kelvin]]. In this law temperature must be expressed on the absolute (Kelvin) scale. The ''displacement'' in Wien's law refers to the way that the position of the peak can be displaced with a change in temperature.<ref name='krane'/> Qualitatively this property can be seen quite simply. As an object is heated, it goes from red-hot to white-hot. This shows that as the temperature is increased, the wavelength that is emitted with the greatest intensity becomes smaller. The wavelength will decrease linearly as the temperature is increased.<ref name='hp'>HyperPhysics. (March 14, 2015). ''Wien's Displacement Law'' [Online]. Available: http://hyperphysics.phy-astr.gsu.edu/hbase/wien.html#c2</ref> Thus, Wien's Law helps to illustrate the connection between colour and temperature. Note that Wien's Law only helps to determine at what wavelength the radiation of a blackbody peaks at. To determine the total energy emitted from the blackbody, the [[Stefan-Boltzmann law]] must be used.
Where <math>\lambda</math> is the wavelength in [[meter]]s, and <math>T</math> is the temperature in [[Kelvin]]. In this law temperature must be expressed on the absolute (Kelvin) scale. The ''displacement'' in Wien's law refers to the way that the position of the peak can be displaced with a change in temperature.<ref name='krane'/> Qualitatively this property can be seen quite simply. As an object is heated, it goes from red-hot to white-hot. This shows that as the temperature is increased, the wavelength that is emitted with the greatest intensity becomes smaller. The wavelength will decrease linearly as the temperature is increased.<ref name='hp'>HyperPhysics. (March 14, 2015). ''Wien's Displacement Law'' [Online]. Available: http://hyperphysics.phy-astr.gsu.edu/hbase/wien.html#c2</ref> Thus, Wien's Law helps to illustrate the connection between colour and temperature. Note that Wien's Law only helps to determine at what wavelength the radiation of a blackbody peaks at. To determine the total energy emitted from the blackbody, the [[Stefan-Boltzmann law]] must be used.
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<html><iframe src="https://phet.colorado.edu/sims/html/blackbody-spectrum/latest/blackbody-spectrum_en.html" width="800" height="600" scrolling="no" allowfullscreen></iframe></html>
<html><iframe src="https://phet.colorado.edu/sims/html/blackbody-spectrum/latest/blackbody-spectrum_en.html" width="800" height="600" scrolling="no" allowfullscreen></iframe></html>
==For Further Reading==
*[[Blackbody radiation]]
*[[Infrared radiation]]
*[[Albedo]]
*Or explore a [[Special:Random|random page]]


==References==
==References==
{{reflist}}
{{reflist}}
[[Category:Uploaded]]
[[Category:Uploaded]]

Revision as of 22:16, 19 January 2020

Figure 1. Blackbody radiation curves for a blackbody at four different temperatures, displaying the shift in peak wavelength for two different temperatures.[1]

Wien's Law, sometimes called Wien's Displacement Law, is a law that determines at what wavelength the intensity of radiation emitted from a blackbody reaches its maximum point.[2] After this point, the intensity decreases as temperature increases. This creates the characteristic shape of blackbody radiation curves. Wien's Law is expressed simply as:[3]

[math] \lambda_{max} \times T = 2.8978 \times 10^{-3} \textrm{m}\cdot\textrm{K} [/math]

Where [math]\lambda[/math] is the wavelength in meters, and [math]T[/math] is the temperature in Kelvin. In this law temperature must be expressed on the absolute (Kelvin) scale. The displacement in Wien's law refers to the way that the position of the peak can be displaced with a change in temperature.[2] Qualitatively this property can be seen quite simply. As an object is heated, it goes from red-hot to white-hot. This shows that as the temperature is increased, the wavelength that is emitted with the greatest intensity becomes smaller. The wavelength will decrease linearly as the temperature is increased.[4] Thus, Wien's Law helps to illustrate the connection between colour and temperature. Note that Wien's Law only helps to determine at what wavelength the radiation of a blackbody peaks at. To determine the total energy emitted from the blackbody, the Stefan-Boltzmann law must be used.

Wien's law is useful in analyzing blackbody curves, but it is also used quite frequently to determine the temperature of hot radiant objects that cannot be easily measured, such as stars.[4]

For more information on Wien's Displacement Law, please see HyperPhysics.

Phet Simulation

The University of Colorado has graciously allowed us to use the following Phet simulation. Explore this simulation to see how the peak wavelength given off by an object changes with temperature.

For Further Reading

References

  1. ↑ "Wien Displacement" Licensed under CC BY-SA 3.0 via Wikimedia Commons - http://commons.wikimedia.org/wiki/File:Wien_Displacement.png#/media/File:Wien_Displacement.png
  2. ↑ 2.0 2.1 Kenneth Krane. Modern Physics, 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.
  3. ↑ Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003.
  4. ↑ 4.0 4.1 HyperPhysics. (March 14, 2015). Wien's Displacement Law [Online]. Available: http://hyperphysics.phy-astr.gsu.edu/hbase/wien.html#c2
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