In radiometry, irradiance is the radiant flux received by a surface per unit area. The SI unit of irradiance is the watt per square metre (symbol W⋅m−2 or W/m2). The CGS unit erg per square centimetre per second (erg⋅cm−2⋅s−1) is often used in astronomy. Irradiance is often called intensity, but this term is avoided in radiometry where such usage leads to confusion with radiant intensity. In astrophysics, irradiance is called radiant flux. Spectral irradiance is the irradiance of a surface per unit frequency or wavelength, depending on whether the spectrum is taken as a function of frequency or of wavelength. The two forms have different dimensions and units: spectral irradiance of a frequency spectrum is measured in watts per square metre per hertz (W⋅m−2⋅Hz−1), while spectral irradiance of a wavelength spectrum is measured in watts per square metre per metre (W⋅m−3), or more commonly watts per square metre per nanometre (W⋅m−2⋅nm−1).
Mathematical definitions
Irradiance Irradiance of a surface, denoted Ee ("e" for "energetic", to avoid confusion with photometric quantities), is defined as
E e = ∂ Φ e ∂ A , {\displaystyle E_{\mathrm {e} }={\frac {\partial \Phi _{\mathrm {e} }}{\partial A}},}
where
∂ is the partial derivative symbol; Φe is the radiant flux received; A is the area. The radiant flux emitted by a surface is called radiant exitance.
Spectral irradiance Spectral irradiance in frequency of a surface, denoted Ee,ν, is defined as
E e , ν = ∂ E e ∂ ν , {\displaystyle E_{\mathrm {e} ,\nu }={\frac {\partial E_{\mathrm {e} }}{\partial \nu }},}
where ν is the frequency. Spectral irradiance in wavelength of a surface, denoted Ee,λ, is defined as
E e , λ = ∂ E e ∂ λ , {\displaystyle E_{\mathrm {e} ,\lambda }={\frac {\partial E_{\mathrm {e} }}{\partial \lambda }},}
where λ is the wavelength.
Property Irradiance of a surface is also, according to the definition of radiant flux, equal to the time-average of the component of the Poynting vector perpendicular to the surface:
E e = ⟨ | S | ⟩ cos α , {\displaystyle E_{\mathrm {e} }=\langle |\mathbf {S} |\rangle \cos \alpha ,}
where
⟨ • ⟩ is the time-average; S is the Poynting vector; α is the angle between a unit vector normal to the surface and S. For a propagating sinusoidal linearly polarized electromagnetic plane wave, the Poynting vector always points to the direction of propagation while oscillating in magnitude. The irradiance of a surface is then given by
E e = n 2 μ 0 c E m 2 cos α = n ε 0 c 2 E m 2 cos α = n 2 Z 0 E m 2 cos α , {\displaystyle E_{\mathrm {e} }={\frac {n}{2\mu _{0}c}}E_{\mathrm {m} }^{2}\cos \alpha ={\frac {n\varepsilon _{0}c}{2}}E_{\mathrm {m} }^{2}\cos \alpha ={\frac {n}{2Z_{0}}}E_{\mathrm {m} }^{2}\cos \alpha ,}
where
Em is the amplitude of the wave's electric field; n is the refractive index of the medium of propagation; c is the speed of light in vacuum; μ0 is the vacuum permeability; ε0 is the vacuum permittivity;
c = 1 ε 0 μ 0 {\textstyle c={\frac {1}{\sqrt {\varepsilon _{0}\mu _{0}}}}}
Z 0 = μ 0 c {\textstyle Z_{0}=\mu _{0}c} is the impedance of free space. This formula assumes that the magnetic susceptibility is negligible; i.e. that μr ≈ 1 (μ ≈ μ0) where μr is the relative magnetic permeability of the propagation medium. This assumption is typically valid in transparent media in the optical frequency range.
Point source A point source of light produces spherical wavefronts. The irradiance in this case varies inversely with the square of the distance from the source.
E = P A = P 4 π r 2 , {\displaystyle E={\frac {P}{A}}={\frac {P}{4\pi r^{2}}},}
where
r is the distance; P is the radiant flux; A is the surface area of a sphere of radius r. For quick approximations, this equation indicates that doubling the distance reduces irradiation to one quarter; or similarly, to double irradiation, reduce the distance to 71%. In astronomy, stars are routinely treated as point sources even though they are much larger than the Earth. This is a good approximation because the distance from even a nearby star to the Earth is much larger than the star's diameter. For instance, the irradiance of Alpha Centauri A (radiant flux: 1.5 L☉, distance: 4.34 ly) is about 2.7 × 10−8 W/m2 on Earth.
Solar irradiance
The global irradiance on a horizontal surface on Earth consists of the direct irradiance Ee,dir and diffuse irradiance Ee,diff. On a tilted plane, there is another irradiance component, Ee,refl, which is the component that is reflected from the ground. The average ground reflection is about 20% of the global irradiance. Hence, the irradiance Ee on a tilted plane consists of three components:
E e = E e , d i r + E e , d i f f + E e , r e f l . {\displaystyle E_{\mathrm {e} }=E_{\mathrm {e} ,\mathrm {dir} }+E_{\mathrm {e} ,\mathrm {diff} }+E_{\mathrm {e} ,\mathrm {refl} }.}
The integral of solar irradiance over a time period is called "solar exposure" or "insolation". Average solar irradiance at the top of the Earth's atmosphere is roughly 1361 W/m2, but at surface irradiance is approximately 1000 W/m2 on a clear day.
SI radiometry units
See also
References