Star+Formation+Test+Problems

=**Star Formation Test Problems**= Pages: Workshop, **Overview**, CADAC, Data Access, Work Area Setup, Path Setup, Utilities, Grid Data, SPH Data, Running, Reporting, LOG

Soft deadline -- by this date you should have the setup (steps 1-4 below) done: **November 15th** Hard deadline -- by this date you should have at least initial results (steps 5-6 below): **November 25th** Mini-Workshop -- during which we will discuss available results and decide how to proceed: **November 26-28**

To participate in this code comparison effort you need to
 * 1) sign up below (just edit this page!)
 * 2) get a CADAC account
 * 3) setup a work area on datastar at SDSC
 * 4) use the supplied utilities to create your grid code or SPH code intial data
 * 5) run the test problems
 * 6) report the results

//**The links provided at the top of each page correspond to these steps; essentially you need to browse them from left to right.**//

Test Problem Definitions
Decaying turbulence from a developed snapshot (one for HD and one for MHD), run for ~2 dynamical times, isothermal, no selfgravity, periodic boundaries. Initial conditions from a grid code at rms Mach ~ 9 and resolution of 1,000^3 are provided both on a grid and as SPH particles, at a number of resolutions (including 256^3, 512^3, 1,024^3), along with utilities that for generating user formatted versions at any resolution. If you run at any resolution above 256^3 you also have to carry out the corresponding lower resolution runs.
 * Problem 1:**

OUTPUT: Please transfer to CADAC 11 snapshots at the following times: 0, 0.02, 0.04, 0.06, ......, 0.2. Time is in units of sound crossing times, L/Cs, with L=1 and Cs=1. **Notice that the velocity in the initial conditions is in units of the sound speed, and that the magnetic field is in units where the magnetic energy is B^2/2.**

DATA ANALYSIS: Power spectra, structure functions, pdfs, computed at CADAC with provided IDL tools (details later).

Same as above, but with selfgravity and sink particles (or selfgravity and some other device to avoid singularities). The strength of selfgravity should be such that g=1000 in the relation
 * Problem 2:**

math \Delta \Phi = g\rho math

OUTPUT: Same as above + sink particle index, age, mass, position, velocity. To allow better tracking of gravitational collapse, 21 snapshots should be transferred, with intervals 0.01; i.e. at 0, 0.01, 0.02, ..., 0.20. Sink particle data should be saved as often as is practical, to allow accurate tracking of positions and accretion rates.

DATA ANALYSIS: Same as above + sink particles mass distribution and accretion histories.


 * Please sign in:**


 * **Name** || **Code** || **Resolution** || **HD/MHD** || **AMR** || **Sinks** || **Present** || **By Tuesday....** ||
 * Åke Nordlund || Stagger-Code || 1,000^3 || HD & MHD || No || Yes || Yes || Problem 1, 500^3 ||
 * Alexei Kritsuk || Enzo || 2,048^3 || HD & MHD || Yes || Yes || Yes || Problem 1, 512^3 ||
 * Daniel Price || Phantom-SPH || 512^3, maybe 1024^3 (particles) || HD & hopefully MHD || No || No || Yes || Problem 1, 256^3 ||
 * Charles Hansen || Orion || 1024^3 || HD || Yes || Yes || No || Problem 1, 512^3 ||
 * Romain Teyssier || RAMSES || 1024^3 || HD & MHD || Yes || hopefully || No ||  ||
 * Anne-Katharina Jappsen || Gadget-2 || to be decided || HD || No || Yes || No ||  ||
 * Jongsoo Kim || TVD or HLL || 1024^3 || HD || No || No || No || Problem 1, 512^3 ||
 * Axel Brandenburg || Pencil Code || 1024^3 || HD & MHD || No || No || Yes || Problem 1, 512^3 ||
 * Mario Flock || PLUTO || 512^3 || HD & MHD || No || No || No ||  ||
 * Christoph Federrath || FLASH || 1024^3 || HD & MHD || Yes || Yes || No || Problem 1, 1024^3 ||
 * Jonathan Carroll || Astrocub || 1024^3 || HD & MHD || No || No || No ||  ||
 * Pak Shing Li || ZEUS-MP || 256^3, 512^3, 1024^3 || HD & MHD || No || No || Yes || Problem 1 ||
 * Hubert Klahr || F-TRAMP || to be decided || HD || No || No || Yes || Problem 1 ||
 * Rolf Kuiper || Petsc || tbd. || HD || No || No || Yes ||  ||
 * Ralf Klessen || Gadget || tbd. || HD || --- || Yes || No || Problem 2 ||
 * Ruben Krasnopolsky || Relaxing TVD || 512^3 || HD & MHD || No || No || Yes ||  ||
 * David Collins || Enzo/PPM-L || 1024^3 || MHD || Maybe || Probably || Yes ||  ||