Greenberger–Horne–Zeilinger state: Difference between revisions

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{{About|the unit of photon flux|the unit of acoustic impedance|Rayl}}
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The '''rayleigh''' is a unit of [[photon]] [[flux]], used to measure [[airglow]] ([[Aurora (astronomy)|aurora]]s, for example). It was first proposed in 1956 by D. M. Hunten, Franklin E. Roach, and J. W. Chamberlain.<ref>{{cite journal | author = Hunten, D. M.; Roach, F. E.; Chamberlain, J. W. | year = 1956 | title= A photometric unit for the airglow and aurora | journal = Journal of Atmospheric and Terrestrial Physics | volume = 8 | pages = 345–346 | doi = 10.1016/0021-9169(56)90111-8 | issue = 6}}</ref> It is named for [[Robert John Strutt, 4th Baron Rayleigh]] (1875–1947).<ref>{{cite journal | doi = 10.1364/AO.13.002160 | first = Doran J. | last = Baker | title = Rayleigh, the Unit for Light Radiance | journal = Applied Optics | volume = 13 | issue = 9 | pages = 2160–2163 | year = 1974 | url = http://www.opticsinfobase.org/abstract.cfm?URI=ao-13-9-2160 | pmid = 20134644|bibcode = 1974ApOpt..13.2160B }}</ref> Its symbol is R (also used for the [[Roentgen (unit)|röntgen]], an unrelated unit). [[SI prefix]]es are used with the rayleigh.
 
One rayleigh (1 R) is defined as a column emission rate of 10<sup>10</sup> photons per [[square metre]] per column per [[second]]. Note that rayleigh is an apparent emission rate, as no allowances have been made for scattering or absorption. The night sky has an intensity of about 250&nbsp;R, while auroras can reach values of 1000&nbsp;kR.
 
The relationship between photon radiance, ''L'', (in units of photons per square metre per second per [[steradian]]) and ''I'' (in units of rayleighs) is simply
 
:<math>I = L \frac{10^{10}}{4\pi}</math>
 
==References==
{{reflist}}
 
[[Category:Photometry]]
[[Category:Units of luminous flux]]
[[Category:Centimetre–gram–second system of units]]

Latest revision as of 21:05, 11 August 2014

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