Programs in Physics & Physical Chemistry
|[Licence| Download | New Version Template] adud_v1_0.tar.gz(991 Kbytes)|
|Manuscript Title: Mie Scattering by Ensembles of Particles with Very Large Size Parameters.|
|Authors: S. Wolf, N.V. Voshchinnikov|
|Program title: miex|
|Catalogue identifier: ADUD_v1_0|
Distribution format: tar.gz
|Journal reference: Comput. Phys. Commun. 162(2004)113|
|Programming language: Fortran 90.|
|Computer: Any machine running standard FORTRAN 90; miex has been tested on an Intel Celeron processor (Redhat Linux 9.0, Intel Fortran Compiler 7.1), an Intel XEON processor (SuSE Linux 9.0, Intel Fortran Compiler 8.0), and a Sun-Blade-1000 (OS 8.5, Sun Workshop Compiler Fortran 90 2.0).|
|Operating system: Redhat Linux 9.0, SuSE Linux 9.0, Sun OS 8.5.|
|RAM: 1MByte to several 100 MByte|
|Keywords: Mie scattering, size parameter, particle ensemble, scattering matrix, Stokes vector, efficiency factor, cross section, asymmetry parameter, albedo.|
Nature of problem:
Among a variety of applications, Mie scattering is of essential importance for the continuum radiative transfer in cosmic dust configurations. In this particular case, Mie theory describes the interaction of electromagnetic radiation with spherical dust grains on the basis of their complex refractive index and size parameter. Both, broad grain size distributions (radii a: nanometers -- millimeters) and a very wide wavelength range (λ ≈ 10-10-10-2m) of the interacting radiation are considered. Previous numerical solutions to the Mie scattering problem are not appropriate to consider size parameters x=2πa/λ > 104 - 105 In contrast to this, the presented code allows to consider arbitrary size parameters. It will be useful not only for applications in astrophysics but also in other fields of science (atmospheric and ocean optics, biophysics, etc.) and industry (particle sizing, ecology control measurements, etc.).
Calculations of Mie scattering coefficients and efficiency factors as outlined by Voshchinnikov , combined with standard solutions of the scattering amplitude functions. Single scattering by particle ensembles is calculated by proper averaging of the respective parameters.
Seconds to minutes.
|||Voshchinnikov N.V. "Optics of Cosmic Dust. I", Astrophysics and Space Physics Reviews 12, 1 (2004)|
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