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Colour of gold-ruby glass, computed for spherical particles with radius 7 nm,

(Experimental data: http://refractiveindex.info/). The scale gives the thickness, multiplied by the density of the particles and the cross section area of a particle.

Mie then writes:

"In contrast to that, e.g. for the rainbow problem, which could be tackled with the method employed here, a pretty large number of partial waves would have to be accounted for and one would encounter very serious computational difficulties."

"Dagegen müßte man z.B. bei dem Regenbogenproblem, das man auch mit der hier angewandten Methode in Angriff nehmen könnte, eine ziemlich große Zahl Partialwellen berücksichtigen und würde auf sehr große rechnerische Schwierigkeiten stoßen." (p. 402)

Nonetheless, the theory has been applied to the rainbow problem. In his standard work[2] on "Light Scattering by Small Particles", H.C. van de Hulst writes 1957: "There is now an impressive body of tabulated numerical results based on the rigorous Mie formulae. […] The bulk of the computations […], terminating in the automatic printing of all Mie coefficients, was made by the electronic ENIAC machine. The Legendre functions π_{n}(θ) and τ_{n}(θ) were computed with an IBM punched card machine. The final multiplications and additions giving the scattering diagram, first complex amplitude, then intensity, were also made on a punched card machine."

The serious computational difficulties have been overcome by skilful programming. In 1983, Bohren and Huffmann published a FORTRAN code in their book [3]. Today, everybody who wants can use this code on a PC and obtain results in a few seconds. There are several websites which offer applications based on the Bohren-Huffmann Mie-subroutine.

Atmospheric phenomena which can be reproduced are rainbows, fogbows, aureoles (or coronae) around the sun or moon, and the glory.

Here are examples:

Averaging over the sun's disc has been performed, and a grey background is assumed with luminosity L=0.4.

Thus the aureole or corona is easily understood by diffraction, and the diffraction pattern of a circular obstacle matches the colours very well.

There is no simple approximation for the colours of the glory, in particular none in terms of ray optics.

Glory and Brocken spectre seen from the Golden Gate Bridge. Photo: "Brocken Inaglory", Source: Wikipedia | Computed solar glory for average droplet radius 8 μm, Gaussian distribution of radii with standard deviation of 1.36 μm. Scale: degrees from antisolar point. |

The subroutine BHMIE requires the input parameters

X: ratio of the circumference of the sphere and the wavelength:

X=2πa/λ_{medium},

where a is the radius of the sphere and λ_{medium} = λ_{vacuum}/n_{medium}

REFREL: the complex index of refraction of the sphere divided by the real index of refraction of the surrounding medium:

REFREL = m_{sphere}/n_{medium},

m_{sphere} = n_{sphere} + i κ_{sphere}

m

NANG is the number of angles from 0 to 90 degree for which the scattering amplitudes are to be computed; NANG > 1.

The subroutine BHMIE returns the quantities S_{1}(θ), S_{2}(θ), Q_{ext}, Q_{sca}, Q_{back}, and G_{sca}.

The complex amplitude functions S_{1}(θ) and S_{2}(θ)
are for the electric field perpendicular and parallel to the scattering plane.
With i_{1} = |S_{1}(θ)|^{2}, i_{2} = |S_{2}(θ)|^{2}, k=2π/λ, one obtains the scattered intensity for incident unpolarized light at a point with polar coordinates r, θ,

I(θ) = 0.5 I_{0} (i_{1}+i_{2}) / (kr)^{2}.

Q_{ext} is the extinction efficiency factor. It is defined as the total effective cross section divided by the geometrical cross section of the scatterer.

The next three quantities are not used in the present context. They are mentioned here only for the sake of completeness.

Q_{sca} is the scattering efficiency. If there is no absorption, it is equal to Q_{ext}, otherwise

Q_{abs} = Q_{ext} – Q_{sca}

Q_{back}, the backscattering efficiency, and

G_{sca} = cos(θ) the averaged cosine of the scattering angle.

For more details, see refs. [2], [3].

The images shown on this page have been obtained using Fortran 77 with extensions, COMPLEX*16 being the most important one. The Open Watcom Fortran 77 compiler has been used.

The output of the codes is an encapsulated PostScript image in all cases. This is a readable Ascii text file and may be edited to satisfy special demands.

**Colloidal metal solutions**

For the colours of colloidal metal solutions, only Q_{ext} is needed, and the program contains the BHMIE subroutine as provided in the Web [4], only MXNANG, the maximum number of angles to be comsidered, is reduced to the minimum value.

**Rainbow, glory, aureole**

The rainbow, glory, and aureole codes use only the scattered intensity. This intensity is normalized to optimize colour rendition on the screen, thus constant factors are omitted, and the quantity

(i_{1}+i_{2}) λ^{2}

is evaluated for a given range of angles. For that purpose, to save computing time and memory, the subroutine BHMIE has been changed to BHMIEMOD, omitting everything which is not needed in this case.

The output of the rainbow code is a coloured bar and a scale giving the angle as measured from the antisolar point. It can be used to compute the glory and the aureole as well. The codes for aureole and glory are derived from the rainbow code, essentially only the graphical output has been changed.

A truncated discretized Gaussian distribution of droplet radii is assumed. The truncation depends on the number "numRad" in the input file giving the total number of radii to be considered. Thus, if numRad = 1, the "Gaussian distribution" consists of only one value. When running the code, it is advisable to start with this value, and with a small droplet radius, to get a feeling for the computing time needed.

Before running the code with a larger value of numRad, one should first set the variable "Test" to "true", t, to see the distribution of radii and weight factors, and to avoid computation of negligible contributions by adjusting numRad.

Colour of colloidal metal solution in transmission: | |

Rainbows and fogbows: rainbow.for, Sample input file: rainbdat.txt | |

Aureole: aureole.for, Sample input file: aureolavedat.txt | |

Glory: glorysRGB.for, Sample input file: glorydat.txt |

Back to the overview, to the section on pigments, on rainbows or on diffraction.

[1] | Gustav Mie: Beiträge zur Optik trüber Medien, speziell kolloidaler Metallösungen. Annalen der Physik, Vierte Folge, Band 25 (1908) 377–445 |

[2] | H.C. van de Hulst: Light Scattering by Small Particles. John Wiley & Sons, Inc, N.Y., 1957 (reprinted 1981, Dover Publications, Inc., New York, ISBN 0-486-64228-3) |

[3] |
C.F. Bohren, D.R. Huffman, Absorption and scattering of light by small particles. John Wiley, New York 1983.
http://onlinelibrary.wiley.com/book/10.1002/9783527618156 |

[4] |
The BHMIE code can be downloaded from these sites: https://code.google.com/p/scatterlib/, http://rime.aos.wisc.edu/MW/models/bhmie.shtml |