en>Dspark76: added see also *Thin-film interference

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	~~{{Refimprove\|date=December 2009}}~~		The name of the writer is Vaughn. What me and my family love is flower arranging but I am have period lately. He is a database administrator. Texas is where her home is but she will have to move one day or 1. Check out her website here: http://ppir.at/stoya80387<br><br>My blog: stoya videos ([http://ppir.at/stoya80387 ppir.at])
	~~{{See also\|Lambertian reflectance}}~~

	In [[optics]], '''Lambert's cosine law''' says that the [[radiant intensity]] or [[luminous intensity]] observed from an ideal [[diffuse reflection\|diffusely reflecting]] surface or ideal diffuse radiator is [[directly proportional]] to the [[cosine]] of the angle θ between the observer's line of sight and the [[Normal (geometry)\|surface normal]].<ref name = "RCAEOH">RCA Electro-Optics Handbook, p.18 ff</ref><ref name="SmithW">Modern Optical Engineering, Warren J. Smith, McGraw-Hill, p.228, 256</ref> The law is also known as the '''cosine emission law'''<ref>{{cite book \| title=Introduction to Optics \| publisher=Prentice Hall \| last=Pedrotti & Pedrotti \| year=1993 \| isbn=0135015456}}</ref> or '''Lambert's emission law'''. It is named after [[Johann Heinrich Lambert]], from his ''[[Photometria]]'', published in 1760.<ref>[http://archive.org/details/lambertsphotome00lambgoog{{cite book\|last=Lambert\|first=J H\|title=Photometria, sive de Mensura et gradibus luminis, colorum et umbrae\|year=1760}}]</ref>

	A surface which obeys Lambert's law is said to be ''Lambertian'', and exhibits [[Lambertian reflectance]]. Such a surface has the same [[radiance]] when viewed from any angle. This means, for example, that to the human eye it has the same apparent brightness (or [[luminance]]). It has the same radiance because, although the emitted power from a given area element is reduced by the cosine of the emission angle, the apparent size (solid angle) of the ~~observed area, as seen by a viewer,~~ is ~~decreased by a corresponding amount~~. ~~Therefore, its radiance (power per unit solid angle per unit projected source area) is the same.~~

	~~==Lambertian scatterers~~ and ~~radiators==~~

	~~When an area element~~ is radiating as a result of being illuminated by an external source, the [[irradiance]] (energy or photons/time/area) landing on that area element will be proportional to the cosine of the angle between the illuminating source and the normal. A Lambertian scatterer will then scatter this light according to the same cosine law as a Lambertian emitter. This means that although the radiance of the surface depends on the angle from the normal to the illuminating source, it will not depend on the angle from the normal to the observer. For example, if the [[moon]] were a Lambertian scatterer, one would expect to see its scattered brightness appreciably diminish towards the [[terminator (solar)\|terminator]] due to the increased angle at which sunlight hit the surface. The fact that it does not diminish illustrates that the moon is not a Lambertian scatterer, and in fact tends to scatter more light into the [[oblique angle]]s than would a Lambertian scatterer.

	~~The emission of a Lambertian radiator does not depend upon the amount of incident radiation,~~ but ~~rather from radiation originating in the emitting body itself. For example, if the [[sun]] were a Lambertian radiator, one would expect to see a constant brightness across the entire solar disc~~. ~~The fact that the sun exhibits [[limb darkening]] in the visible region illustrates that it~~ is ~~not~~ a ~~Lambertian radiator~~. ~~A [[black body]]~~ is ~~an example of a Lambertian radiator.~~

	~~==Details of equal brightness effect==~~

	~~<div style="float: right">~~
	{\|
	\|-
	~~\| [[Image:Lambert Cosine Law 1.svg\|frame\|right\|Figure 1: Emission rate (photons/s) in a normal and off-normal direction. The number of photons/sec directed into any wedge~~ is ~~proportional~~ to ~~the area of the wedge.]]~~
	\|-
	\| [[Image:Lambert Cosine Law 2.svg\|frame\|right\|Figure 2: Observed intensity (photons/(s·cm<sup>2</sup>·sr)) for a normal and off-normal observer; ''dA''<sub>0</sub> is the area of the observing aperture and ''dΩ'' is the solid angle subtended by the aperture from the viewpoint of the emitting area element.]]
	\|}
	~~</div>~~
	~~The situation for a Lambertian surface (emitting~~ or ~~scattering) is illustrated in Figures~~ 1 ~~and 2~~. For conceptual clarity we will think in terms of [[photon]]s rather than [[energy]] or [[luminous energy]]. The wedges in the [[circle]] each represent an equal angle ''dΩ'', and for a Lambertian surface, the number of photons per second emitted into each wedge is proportional to the area of the wedge.

	It can be seen that the length of each wedge is the product of the [[diameter]] of the circle and cos(''θ''). It can also be seen that the maximum rate of photon emission per unit [[solid angle]] is along the normal and diminishes to zero for ''θ'' = 90°. In mathematical terms, the [[radiance]] along the normal is ''I'' photons/(s·cm<sup>2</sup>·sr) and the number of photons per second emitted into the vertical wedge is ''I'' ''dΩ'' ''dA''. The number of photons per second emitted into the wedge at angle ''θ'' is ''I'' cos(''θ'') ''dΩ'' ''dA''.

	Figure 2 represents what an observer sees. The observer directly above the area element will be seeing the scene through an aperture of area ''dA''<sub>0</sub> and the area element ''dA'' will subtend a (solid) angle of ''dΩ''<sub>0</sub>. We can assume without loss of generality that the aperture happens to subtend solid angle ''dΩ'' when "viewed" from the emitting area element. This normal observer will then be recording ''I'' ''dΩ'' ''dA'' photons per second and so will be measuring a radiance of
	:~~<math>~~
	~~I_0=\frac{I\, d\Omega\, dA}{d\Omega_0\, dA_0}~~
	~~</math> photons~~/~~(s·cm<sup>2<~~/~~sup>·sr)~~.

	~~The observer~~ at ~~angle ''θ'' to the normal will be seeing the scene through the same aperture of area ''dA''<sub>0<~~/~~sub> and the area element ''dA'' will subtend a (solid) angle of ''dΩ''~~<~~sub~~>0<~~/sub~~>~~ cos(''θ''). This observer will be recording ''I'' cos(''θ'') ''dΩ'' ''dA'' photons per second, and so will be measuring a radiance of~~

	:~~<math>~~
	~~I_0=\frac{I \cos~~(~~\theta)\, d\Omega\, dA}{d\Omega_0\, \cos(\theta)\, dA_0}~~
	~~=\frac{I\, d\Omega\, dA}{d\Omega_0\, dA_0}~~
	~~</math> photons/(s·cm<sup>2</sup>·sr),~~

	~~which is the same as the normal observer.~~

	~~== Relating peak luminous intensity and luminous flux ==~~

	~~In general, the~~ [[luminous intensity]] of a point on a surface varies by direction; for a Lambertian surface, that distribution is defined by the cosine law, with peak luminous intensity in the normal direction. Thus when the Lambertian assumption holds, we can calculate the total [[luminous flux]], <math>F_{tot}</math>, from the peak [[luminous intensity]], <math>I_{max}</math>, by integrating the cosine law:
	~~:<math>F_{tot} = \int\limits_0^{\pi/2}\,\int\limits_0^{2\pi}\cos(\theta)I_{max}\,\sin(\theta)\,\operatorname{d}\phi\,\operatorname{d}\theta </math>~~
	:~~::<math>= 2\pi\cdot I_{max}\int\limits_0^{\pi~~/~~2}\cos(\theta)\sin(\theta)\,\operatorname{d}\theta <~~/~~math>~~
	~~:::<math>= 2\pi\cdot I_{max}\int\limits_0^{\pi/2}\frac{\sin(2\theta)}{2}\,\operatorname{d}\theta </math>~~
	~~and so~~
	~~:<math>F_{tot}=\pi\,\mathrm{sr}\cdot I_{max}</math>~~
	~~where <math>\sin(\theta)</math> is the determinant of the [[Jacobian matrix]] for the [[unit sphere]], and realizing that <math>I_{max}</math> is luminous flux per [[steradian]]~~.~~<ref>Incropera and DeWitt, ''Fundamentals of Heat and Mass Transfer'', 5th ed., p.710.</ref> Similarly, the peak intensity will be <math>1~~/~~(\pi\,\mathrm{sr})</math> of the total radiated luminous flux~~. For Lambertian surfaces, the same factor of <math>\pi\,\mathrm{sr}</math> relates [[luminance]] to [[luminous emittance]], [[radiant intensity]] to [[radiant flux]], and [[radiance]] to [[radiant emittance]].{{citation needed\|date=June 2013}} Radians and steradians are, of course, dimensionless and so "rad" and "sr" are included only for clarity.

	Example: A surface with a luminance of say 100 cd/m<sup>2</sup> (= 100 nits, typical PC monitor) will, if it is a perfect Lambert emitter, have a luminous emittance of 314 lm/m<sup>2</sup>. If its area is 0.1 m<sup>2</sup> (~19" monitor) then the total light emitted, or luminous flux, would thus be 31.4 lm.

	~~== Uses ==~~

	~~Lambert's cosine law in its reversed form ([[Lambertian reflection~~]~~]) implies that the apparent brightness of a [[Lambertian surface]] is proportional to the cosine of the angle between the surface normal and the direction of the incident light.~~

	~~This phenomenon is, among others, used when creating [[Molding (decorative~~)\|mouldings]], which are a means of applying light- and dark-shaded stripes to a structure or object without having to change the material or apply [[pigment]]. The contrast of dark and light areas gives definition to the object. Mouldings are strips of material with various cross-sections used to cover transitions between surfaces or for decoration.

	~~==See also==~~
	* [[Transmittance]]
	* [[Reflectivity]]
	* [[Passive solar building design]]
	* [[Sun path]]

	~~== References ==~~
	~~<references/>~~

	~~{{DEFAULTSORT:Lambert's Cosine Law}}~~
	~~[[Category:Radiometry]]~~
	~~[[Category:Photometry]]~~
	~~[[Category:3D computer graphics]]~~
	~~[[hu:Lambert-féle koszinusz törvény]]~~

	~~[[es:Ley de Beer-Lambert]]~~
	~~[[zh:餘弦輻射體]]~~

en>Ramaksoud2000: Reverted edit(s) by 117.206.51.77 identified as test/vandalism using STiki

2013-04-20T01:07:46Z

Reverted edit(s) by 117.206.51.77 identified as test/vandalism using STiki

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en>Jarble at 19:17, 1 September 2012

2012-09-01T19:17:16Z

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en>Dspark76: added see also *Thin-film interference

en>Ramaksoud2000: Reverted edit(s) by 117.206.51.77 identified as test/vandalism using STiki

en>Jarble at 19:17, 1 September 2012