PROGRAM SUMMARY
Title of program:
MC3D
Catalogue identifier:
ADMH
Ref. in CPC:
132(2000)166
Distribution format: tar gzip file
Operating system: Compaq TruUnix 4.0F, SuSE Linux V4.3 ... V6.3
High speed store required:
50MK words
Number of bits in a word:
8
Number of lines in distributed program, including test data, etc:
61382
Keywords:
Astrophysics, Radiative transfer, Interstellar matter,
Circumstellar shells.
Programming language used: Fortran
Computer:
Alpha Workstation ,
Intel Pentium/Pentium II.
Nature of problem:
For the interpretation of spectra, images, and polarization maps of
young stellar objects (YSO) and active galactic nuclei (AGN), radiative
transfer simulations provide the necessary basis. Nowadays, for the
interpretation of very high-resolution maps, there exists a strong need
for a code which solves the radiative transfer problem even in the case
of very complex model configurations (e.g., clumpy dust density
distributions, binary systems, direct usage of dust density
distributions obtained from hydrodynamical simulations).
Method of solution:
The radiative transfer problem is solved with the help of the
Monte-Carlo method. The radiatve energy is partitioned in so-called
test photons. Scattering, absorption and re-emission processes by
spherical dust grains are considered. Images, polarization maps, and
spectral energy distributions (SED) of the considered objects can be
obtained.
Restrictions:
The program as presented can handle one dust component defined by a
certain radius and chemical composition. However, this is not a
principal restriction. It works best for dust density configurations
with an optical depth of about tau=10**-3 ... 10**+3.
Typical running time:
The typical running time of the program depends on the complexity of the
problem and the geometry of the model. It amounts to several minutes
... several hours.
Unusual features:
None