Rayleigh (unit) explained

The rayleigh is a unit of photon flux, used to measure faint light emitted in the sky, such as airglow and auroras. It was first proposed in 1956 by Donald M. Hunten, Franklin E. Roach, and Joseph W. Chamberlain.^[1] It is named for Robert Strutt, 4th Baron Rayleigh (1875–1947).^[2] Its symbol is R (also used for the röntgen, an unrelated unit). SI prefixes are used with the rayleigh.

One rayleigh (1 R) is defined as a column emission rate of 10¹⁰ photons per square metre per column per second. The rayleigh is a unit of an apparent emission rate, without allowances being made for scattering or absorption. The night sky has an intensity of about 250 R, while auroras can reach values of 1000 kR.

The relationship between photon radiance, L, (with unit photon per square metre per second per steradian) and I (with unit rayleigh) is$$I\; =\; 4\backslash pi~\backslash mathrm\; \backslash times\; L\; \backslash times\; \backslash frac$$

Notes and References

1. Hunten, D. M. . Franklin E. Roach . Roach, F. E. . Chamberlain, J. W. . 1956 . A photometric unit for the airglow and aurora . Journal of Atmospheric and Terrestrial Physics . 8 . 345–346 . 10.1016/0021-9169(56)90111-8 . 6 . 1956JATP....8..345H .
2. 10.1364/AO.13.002160 . Doran J. . Baker . Rayleigh, the Unit for Light Radiance . Applied Optics . 13 . 9 . 2160–2163 . 1974 . 20134644 . 1974ApOpt..13.2160B .