HO-CHUNK: 3-D Radiation Transfer Codes:

Contributors include Kenny Wood, Jon Bjorkman, and Mike Wolff

Star Formation modeling codes:

(see below for instructions for installing)

1.  HO-CHUNK.ttsscat.20041209, calculates scattering and polarization in protostellar geometries (star surrounded by disk and/or envelope, bipolar cavities, outflows);  good for computing optical/near-IR images where most of the emitted radiation comes from the central star and then scatters in the disk+envelope.  Latest update:  December 9, 2004.  The history of changes are listed here.

2.  HO-CHUNK.ttsre.20070405, calculates radiative equilibrium temperature solution, thermal emission, scattering and polarization in protostellar geometries;  good for computing spectral energy distributions (SEDs), polarization spectra, and thermal images.   Latest update:  April 5, 2007.  The history of changes are listed here.  Note:  we no longer supply a set of Kurucz and Nextgen atmosphere models because they are available on the protostars website . 

More general circumstellar codes:

3.  HO-CHUNK.sphere.20040407, calculates scattering and polarization in circumstellar dust or electrons illuminated by a central source;  good for computing optical/near-IR images.  It's currently set up to compute an ellipsoidal envelope and/or a disk.  The instructions explain how you can modify the geometry.  Note: this code will be replaced by "csscat" within a few months.  It will do the same thing, just will derive from the ttsscat program and will be easier to maintain.  Anyway "sphere" is misnomer since it does 2-D and 3-D geometries.

4.  HO-CHUNK.csre.20050228, calculates radiative equilibrium temperature solution, thermal emission, scattering and polarization in circumstellar dust illuminated by a central source;  good for computing SEDs, polarization spectra and thermal images.   It's currently set up to compute an ellipsoidal envelope and/or a disk.  The instructions explain how you can modify the geometry.   The history of changes are listed here.

Learning tools:

Here is a manual that describes Monte Carlo radiation transfer.

5.  sphere_1d.20040407.  this does isotropic scattering in a sphere.  You can vary the radial density profile.  this is almost too boring a code.  But it computes intensity moments vs radius which seems to excite some people. 

6.  slab.20040407, this is a plane-parallel code that computes isotropic scattering.  It computes intensity moments as a function of optical depth and emergent intensity as a function of angle.  If you want to learn monte carlo, this might be the best starting point.  It has the fewest lines of code.

7.  blob.20040407, this computes scattering and polarization off a spherical distribution of particles.  can be used to compute scattering off a planet for example.   This is a good learning tool if you want to learn how to do polarization (though if you want to see more clever coding, ask Jon Bjorkman for his routines).  (and I haven't tried to clean up the code, sorry).

There are also some codes available on Kenny Wood's webpage.

Available soon:

8.  ttsre_hseq, calculates the hydrostatic density structure of the disk as well as radiative equilibrium solution for temperature.


Instructions:

All of these programs come as a gzipped tar file (e.g., ttsscat.tar.gz).  here's the easiest way to install, with ttsscat as example:

(download the file, click on the above link)
mkdir ttsscat
mv ttsscat.[date].tar.gz ttsscat
cd ttsscat
tar -xzf ttsscat.tar.gz

this will create several directories and, most important, an instructions.txt file.  that should take you through the rest.  All the programs come with sample runs and plotting files (using IDL).  They've been tested most extensively using Linux compilers, g77 and LF95 (yes, they are fortran 77 codes).   We've just started running the radiative equilibrium code (ttsre) under Mac OSX using the g77, IBM XLF, and Absoft compilers and that seems to work fine.   

Contact me with questions, comments, bugs, improvements, etc.:  bwhitney@spacescience.org