Wiens Law - Revision history

Jmdonev: 1 revision imported

2020-01-31T05:10:07Z

1 revision imported

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Energy>Jmdonev at 22:16, 19 January 2020

2020-01-19T22:16:16Z

← Older revision		Revision as of 22:16, 19 January 2020
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	[[Category:Done ~~2015~~-04-01]]		[[Category:Done 2020-01-31]]
			[[Category:Brodie edit]]
	[[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]]

Jmdonev at 22:15, 19 January 2020

2020-01-19T22:15:19Z

← Older revision		Revision as of 22:15, 19 January 2020
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	The [http://phet.colorado.edu/ 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.		The [http://phet.colorado.edu/ 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.

	<html><iframe src="~~http~~://phet.colorado.edu/sims/blackbody-spectrum/blackbody-spectrum_en.html" width="800" height="600"></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>

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

Jmdonev: Jmdonev moved page Wien's Law to Wiens Law without leaving a redirect: apostrophe problem

2020-01-19T22:14:26Z

Jmdonev moved page Wien's Law to Wiens Law without leaving a redirect: apostrophe problem

← Older revision	Revision as of 22:14, 19 January 2020
(No difference)

Jmdonev at 19:32, 13 June 2018

2018-06-13T19:32:54Z

← Older revision		Revision as of 19:32, 13 June 2018
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	<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} mK </math></center>

	Where <m>\lambda</m> is the wavelength in [[meter]]s, and <m>T</m> 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.

	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.<ref name='hp'/>		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.<ref name='hp'/>

Jmdonev at 19:32, 13 June 2018

2018-06-13T19:32:30Z

← Older revision		Revision as of 19:32, 13 June 2018
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	<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><m> \lambda_{max} \times T = 2.8978 \times 10^{-3} mK </m></center>		<center><math> \lambda_{max} \times T = 2.8978 \times 10^{-3} mK </math></center>

	Where <m>\lambda</m> is the wavelength in [[meter]]s, and <m>T</m> 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 <m>\lambda</m> is the wavelength in [[meter]]s, and <m>T</m> 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.

J.williams: 1 revision imported

2015-08-26T21:31:48Z

1 revision imported

← Older revision	Revision as of 21:31, 26 August 2015
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J.williams at 17:00, 12 August 2015

2015-08-12T17:00:33Z

New page

[[Category:Done 2015-04-01]]
[[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>

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

Where <m>\lambda</m> is the wavelength in [[meter]]s, and <m>T</m> 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.

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.<ref name='hp'/>

For more information on Wien's Displacement Law, please see [http://hyperphysics.phy-astr.gsu.edu/hbase/wien.html#c2 HyperPhysics].
==Phet Simulation==
The [http://phet.colorado.edu/ 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.

<html><iframe src="http://phet.colorado.edu/sims/blackbody-spectrum/blackbody-spectrum_en.html" width="800" height="600"></iframe></html>

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