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 Wâ m<sup>âÂÂ2</sup> or W/m<sup>2</sup>). The CGS unit erg per square centimetre per second (ergâ cm<sup>âÂÂ2</sup>â s<sup>âÂÂ1</sup>) 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 (Wâ m<sup>âÂÂ2</sup>â Hz<sup>âÂÂ1</sup>), while spectral irradiance of a wavelength spectrum is measured in watts per square metre per metre (Wâ m<sup>âÂÂ3</sup>), or more commonly watts per square metre per nanometre (Wâ m<sup>âÂÂ2</sup>â nm<sup>âÂÂ1</sup>).
Irradiance of a surface, denoted E<sub>e</sub> ("e" for "energetic", to avoid confusion with photometric quantities), is defined as
where
The radiant flux emitted by a surface is called radiant exitance.
Spectral irradiance in frequency of a surface, denoted E<sub>e,ý</sub>, is defined as
where ý is the frequency.
Spectral irradiance in wavelength of a surface, denoted E<sub>e,û</sub>, is defined as
where û is the wavelength.
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:
where
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
where
This formula assumes that the magnetic susceptibility is negligible; i.e. that ü<sub>r</sub> â 1 (ü â ü<sub>0</sub>) where ü<sub>r</sub> is the relative magnetic permeability of the propagation medium. This assumption is typically valid in transparent media in the optical frequency range.
A point source of light produces spherical wavefronts. The irradiance in this case varies inversely with the square of the distance from the source.
where
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<sub>âÂÂ</sub>, distance: 4.34 ly) is about 2.7 à10<sup>âÂÂ8</sup> W/m<sup>2</sup> on Earth.
The global irradiance on a horizontal surface on Earth consists of the direct irradiance E<sub>e,dir</sub> and diffuse irradiance E<sub>e,diff</sub>. On a tilted plane, there is another irradiance component, E<sub>e,refl</sub>, which is the component that is reflected from the ground. The average ground reflection is about 20% of the global irradiance. Hence, the irradiance E<sub>e</sub> on a tilted plane consists of three components:
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/m<sup>2</sup>, but at surface irradiance is approximately 1000 W/m<sup>2</sup> on a clear day.