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tests:collision:gc1_archive

This is an old revision of the document!

# Archived from Gaia Challenge 1

## Other possible challenges

### Pal 5 model from Andreas Kuepper in streams section

Same analyses as in Challenge 2 and 3, but with cluster on eccentric orbit and “polluting” stars from tidal tails. The models posted in the streams section were not evolved with stellar evolution and for a Hubble time, but Andreas sent me files for that. Will upload them if there is interest.

### Models with initial rotation

Different models with angular momentum are within the group: collapsing spheres, cold fractal collapse, cluster mergers.

#### Collapse of homogeneous spheres with angular momentum

Below snapshots of 3 cold(ish) collapses of homogeneous spheres with angular momentum. Initial virial ratios and angular momentum were taken from the 3 models described in Gott (1972). The models contain 2e5 stars, a Kroupa IMF between 0.1 and 100 Msun and snapshots are at t=30 [NBODY]. The amount of rotation is quantified with Peebles parameter in the title:

1. rot_collapse_lam0.127.gz NEW! Tuesday August 20
2. rot_collapse_lam0.168.gz NEW! Tuesday August 20
3. rot_collapse_lam0.212.gz NEW! Tuesday August 20

#### Mergers

Merger between 2 clusters of equal mass, equal containing 1e5 stars, a Kroupa IMF between 0.1 and 100 Msun. The initial orbit of the cluster pair had zero energy and different angular momentum. The

1. rot_merger_lam0.128.gz NEW! Tuesday August 20

For both collapse and mergers collapse contain:

[] [NBODY] [NBODY]

#### Collapse of non-homogeneous spheres with angular momentum

(Based on simulations ran by Anna Lisa Varri, see Ref1 Ref2)

Below snapshots of two cold(ish) collapses of isolated spheres with N=64k, equal mass stars, non-homogeneous initial density distribution (fractal dimension D = 2.8, 2.4, as in the file name), and approximate solid-body rotation. The configurations are characterized by the same initial values of virial ratio and global angular momentum as in the homogeneous case #3 (with ). The simulations have been performed with STARLAB and the snapshots are taken at T=20 [NBODY].

1. rot_collapse_fracd2.4.gz NEW! Tuesday August 20
2. rot_collapse_fracd2.8.gz NEW! Tuesday August 20

The file header contains: N, T, coordinates and velocities of the center of mass. The file format is as follow:

[NBODY] [NBODY] [NBODY]

### More ideas (but no mock data for these yet)

1. What is the effect of binary stars?
1. Is there a dynamical “smoking gun” for an intermediate mass black hole?