Storyboard

The propagation of light in a homogeneous medium occurs rectilinearly at a characteristic speed that depends on both the medium and the frequency (color) of the light.

Propagation can be described both as a corpuscular model, in which the particles are called photons, as a wave model.

>Model

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Light is an electromagnetic wave with a wavelength $\lambda$ that falls within the range of 380 nm to 750 nm, encompassing the visible spectrum that our eyes can perceive.

Light propagates in a straight line and can undergo refraction, meaning it can be deviated, if the speed of light changes due to the medium it passes through.

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Light travels in a straight line and radiates spherically around its source.

Because of this spherical distribution, its intensity decreases with distance from the source.

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When light passes through an aperture, it does not propagate uniformly but instead exhibits a distribution, creating what is known as a penumbra.

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Parameters

$\theta$

theta

Angulo respecto a la dirección del haz

rad

$\Omega$

Omega

Angulo solido

-

$r$

r

Distancia a la fuente

m

$r_1$

r_1

Distancia a la fuente 1

m

$r_2$

r_2

Distancia a la fuente 2

m

$\Delta\Omega$

DOmega

Elemento de angulo solido

-

$\Delta\Phi$

DPhi

Elemento de flujo lumínico

J

$\Phi$

Phi

Flujo lumínico total

J

$I_1$

I_1

Intensidad de la luz 1

W/m^2

$I_2$

I_2

Intensidad de la luz 2

W/m^2

$E$

E

Irradiancia

lx

$I$

I

Light Intensity

W/m^2

Variables

Calculations

• Alternative method
• Traditional method
• Strategy
• 2D
• 3D

Equation

Number

First, select the equation: to , then, select the variable: to

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Calculations

Symbol

Equation

Solved

Translated

Calculations

Symbol

Equation

Solved

Translated

Variable Given Calculate Target : Equation To be used

Equations

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Equation

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If light emits in all directions uniformly, it will distribute itself evenly over the surface of an imaginary sphere with an area of

$4\pi r^2$

Hence, if we know its intensity at a distance $r_1$, we can predict its intensity at a distance $r_2$ using

$I_2 =\displaystyle\frac{ r_1 ^2}{ r_2 ^2} I_1$

Conditions

Variables

$r_1$

Distancia a la fuente 1

$m$

9829

$r_2$

Distancia a la fuente 2

$m$

9830

$I_1$

Intensidad de la luz 1

$W/m^2$

9831

$I_2$

Intensidad de la luz 2

$W/m^2$

9832

Relation

Development

Since the amount of light is conserved, the intensity (energy per area) multiplied by the area must be a constant, which leads us to the following relationship:

$4\pi r_1^2I_1=4\pi r_2^2I_2$

Therefore, we can express the relationship between intensities at different distances as:

$I_2 =\displaystyle\frac{ r_1 ^2}{ r_2 ^2} I_1$

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Equation

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Radiative flux ($\Phi$) is calculated from the intensity (I) and the solid angle ($d\Omega$) being considered, using the formula:

$\Delta\Phi = I \Delta\Omega$

Conditions

Variables

$\Delta\Omega$

Elemento de angulo solido

$-$

9834

$\Delta\Phi$

Elemento de flujo lumínico

$J$

9833

$I$

Light Intensity

$W/m^2$

5140

Relation

and it is measured in watts (W).

In the context where flux is evaluated with respect to the human eye's ability to perceive luminous power, it is expressed in the unit of lumens (lm).

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Equation

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Since the flux through an element of angle $d\Omega$ is defined as

the total flux is obtained by integrating the intensity over the entire surface, as shown in the following expression:

$\Phi =\displaystyle\int I d \Omega$

Conditions

Variables

$\Omega$

Angulo solido

$-$

9828

$\Phi$

Flujo lumínico total

$J$

9827

$I$

Light Intensity

$W/m^2$

5140

Relation

Development

Si se quiere conocer el flujo total se debe sumar sobre toda la superficie. Esto es se debe integrar (=sumar) sobre toda la superficie de modo de

$\Delta\Phi = I \Delta\Omega$

lo que arroja

$\Phi =\displaystyle\int I d \Omega$

Some examples of total flux include:

Source | Flux

High-Pressure Xenon Lamp | 3.0E+6 lm

Arc Lamp | 1.0E+4 lm

65W Fluorescent Lamp | 3.3E+3 lm

60W Bulb | 6.2E+2 lm

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Equation

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When radiation with intensity I strikes a surface at an angle \theta relative to the direction of incidence, the irradiance, denoted as

$E=\displaystyle\frac{I\cos\theta}{r^2}$

Conditions

Variables

$\theta$

Angulo respecto a la dirección del haz

$rad$

9826

$r$

Distancia a la fuente

$m$

9825

$E$

Irradiancia

$lx$

9824

$I$

Light Intensity

$W/m^2$

5140

Relation

is measured in Lux (lx), which corresponds to one lumen per square meter.

For natural light, the following values can be used as reference:

Scenario Irradiance

Noon, summer, sunny 1.0E+5 lx

Noon, summer, cloudy 2.0E+4 lx

Noon, winter, sunny 1.0E+4 lx

Noon, winter, cloudy 2.0E+3 lx

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