Importance of the initial conditions for star formation

The initial conditions play an important role in star formation. Both the initial turbulent motions as well as the density configuration determine the fragmentation of the gas as well as the formation of protostars and accretion onto them. The three papers associated with our work are

The video shows the comparison between two density profiles with the same initial turbulent velocity fields. On the density is set up as a scales Bonnor-Ebert sphere, on the right the gas follows a power-law distribution with index -1.5.

other video formats avi (8MB), mov (3.2MB)

Sink particle data

The stars are Lagrangian sink particles that move relative to the grid and are able to accrete gas. For follow-up studies and comparison projects we provide the sink particle data. The files include the following entries for every sink particle and every time step

simulation density profile turbulence seed data file
TH-m-1 top hat mixed 1bzip2 (40 MB)
TH-m-2 top hat mixed 2bzip2 (61 MB)
BE-c-1 BE sphere compressive1bzip2 (45 MB)
BE-c-2 BE sphere compressive2bzip2 (44 MB)
BE-m-1 BE sphere mixed 1bzip2 (30 MB)
BE-m-2 BE sphere mixed 2bzip2 (35 MB)
BE-s-1 BE sphere solenoidal 1bzip2 (26 MB)
BE-s-2 BE sphere solenoidal 2bzip2 (42 MB)
PL15-c-1power-law, 1.5compressive1bzip2 (96 MB)
PL15-c-2power-law, 1.5compressive2bzip2 (125 MB)
PL15-m-1power-law, 1.5mixed 1bzip2 (5 MB)
PL15-m-2power-law, 1.5mixed 2bzip2 (80 MB)
PL15-s-1power-law, 1.5solenoidal 1bzip2 (5 MB)
PL15-s-2power-law, 1.5solenoidal 2bzip2 (145 MB)
PL20-c-1power-law, 2.0compressive1bzip2 (3 MB)

You can also download all files (bzip2, 782 MB). There is also a small C++ program that helps reading in the files and does a basic sorting of the data (tar, 24kB).