Computer Physics Communications Program Library

Programs in Physics & Physical Chemistry

PROGRAM SUMMARY

Manuscript Title: Debris Disk Radiative Transfer Simulation Tool (DDS)
Authors: S. Wolf, L. A. Hillenbrand
Program title: Debris Disk Radiative Transfer Simulator (DDS)
Catalogue identifier: ADVV
Journal reference: Comput. Phys. Commun. 171(2005)208
Programming language: Fortran 90 (for the main program; furthermore Perl, CGI and HTML).
Computer: PC with Intel(R) XEON(TM) 2.80 GHz processor.
Operating system: SUSE Linux 9.1.
RAM: 10⁸ words
Word size: 8 bits
Keywords: Radiative transfer, dust, absorption, scattering, debris disk - astrophysics.
PACS: 94.10.Gb, 97.21.+a, 97.82.+k.
Classification: 1.3.
Nature of problem: Simulation of scattered light and thermal reemission in arbitrary optically dust distributions with spherical, homogeneous grains where the dust parameters (optical properties, sublimation temperature, grain size) and SED of the illuminating/ heating radiative source can be arbitrarily defined (example application: Wolf and Hillenbrand 2003). The program is optimized for studying circumstellar debris disks where large grains (i.e., with large size parameters) are expected to determine the far-infrared through millimeter dust reemission spectral energy distribution.
Solution method: Calculation of the dust temperature distribution and dust reemission and scattering spectrum in the optically thin limit.
Restrictions: The approach to calculate dust temperatures and dust reemission spectra is only valid in the optically thin regime. The validity of this constraint is verified for each model during the runtime of the code. The relative abundances of different grains can be arbitrarily chosen, but must be constant outside the dust sublimation region., i.e., the shape of the (arbitrary) radial dust density distribution outside the dust sublimation region is the same forall grain sizes and chemistries. The size of upload files (such as the dust density distribution, optical data of the dust grains, stellar spectral energy distribution, etc.) is limited (see http://aida28.mpiahd.mpg.de/~swolf/dds/ for current file size limits). However, the resulting limitation to the complexity of possible model definitions is marginal only.
Unusual features: The program as provided through the CPC Program Library is equipped with an HTML user interface. It is installed and available at http//aida28.mpia-hd.mpg.de/~swolf/dds.
Running time: 3 sec - 30 min (depending on the complexity of the model)
References:
[1]	Wolf, S., Hillenbrand, L.A., 2003, Astroph. Journal, 596, 603 3