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


Problem 1:
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.

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).

Problem 2:
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



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