RADMC-3D Version 2.0
Introduction
RADMC-3D is a tool for astrophysical research. It computes the observational appearance of an astrophysical object on the sky of the observer. It solves the non-local radiative transfer problem of dusty media, including thermal radiative transport and scattering.
For a very long time (from its inception in 2007 to 2020) it had a version number smaller than 1, because it contained numerous modes and features that were still experimental. The latest (and longest lasting) version was 0.41. But it was high time to make a new version. I decided to skip version 1, because that would give the impression that the code is still new. So we go straight to version 2.
Compared to version 0.41, the new version 2.0 is not very different. The basic Fortran-90 code is still the same. This means that you can use version 2.0 without having to worry that the new version has potential new bugs that were introduced since 0.41. Having said that: it does not mean that verion 2.0 is bug-free.
What is new in version 2.0 is some of the Python front- and back-end. I also removed old stuff that is no longer necessary. And in version 2.0 IDL front/back-end is no longer supported (if you don't know what IDL is, no need to worry).
How to use RADMC-3D
To learn what can be done with RADMC-3D and how to use it, please consult the extensive manual in the directory manual/. This manual is written using Sphinx, and therefore has a latex version (manual/sphinx/_build/latex/radmc3d.pdf) and an HTML version (manual/sphinx/_build/html/index.html).
Simple example models are found in the examples/ directory. The README files in these directories explain how to run the models.
Website
For more information, please consult the website http://www.ita.uni-heidelberg.de/~dullemond/software/radmc-3d