## "2D Fokker-Planck models of rotating clusters" |
---|

Where

and

(cylindrical coordinates were used)The initial models are rotating King models of the form

Where:

,

Initial conditions are determined by:

,dimensionless angular velocity (rotating parameter)

,dimensionless potential (King parameter)

The age of the system is given in units of the initial half mass relaxation time:

The dynamical ellipticity is calculated following Goodman (1983), given by

Where

Initial parameters of the 12 rotating cluster models.

King parameter Wo | rotating parameter ωo | |||
---|---|---|---|---|

3.0 | 0.0 | 0.30 | 0.60 | 0.90 |

6.0 | 0.0 | 0.30 | 0.60 | 0.90 |

9.0 | 0.0 | 0.06 | 0.08 | 0.10 |

Evolution grid in interval coordinates for the 12 models. The cells contain the total number of datasets available for the grid point with given time and ellipticity.

Ellipticity | Time (t/trh) | |||||
---|---|---|---|---|---|---|

(0,2) | (2,4) | (4,6) | (6,8) | (8,10) | (10,12) | |

(0.00-0.02) | 59 | 16 | 40 | 93 | 58 | 58 |

(0.02-0.04) | 5 | 24 | 15 | 10 | ||

(0.04-0.06) | 8 | 27 | 9 | 14 | ||

(0.06-0.10) | 28 | 62 | 11 | 2 | ||

(0.10-0.15) | 19 | 24 | 3 | |||

(0.15-0.20) | 6 | 7 | ||||

(0.20-0.25) | 4 | |||||

(0.25-0.30) | 5 | |||||

(0.30-0.50) | 3 |

We present the evolution in time of global parameters, classified by initial King- and rotating parameters (see description below)

Model (Wo, ωo) | Datafiles |
---|---|

(3,0.00) | time030_000 |

(3,0.30) | time030_030 |

(3,0.60) | time030_060 |

(3,0.90) | time030_090 |

(6,0.00) | time060_000 |

(6,0.30) | time060_030 |

(6,0.60) | time060_060 |

(6,0.90) | time060_090 |

(9,0.00) | time090_000 |

(9,0.06) | time090_006 |

(9,0.08) | time090_008 |

(9,0.10) | time090_010 |

Description of data:

Column 1: Time(t/t_rh) THTIO

Column 2: Timestep NSTEP

Column 3: Time (t/t_rc) TCTIO

Column 4: Core radius RCORE

Column 5: Central density XRHO(1,1)

Column 6: Central rotational velocity VROT(1,1)

Column 7: Central 1-dim Velocity dispersion XSIGT(1,1)

Column 8: Ellipticity EDYN

Column 9: Escape energy SEE

Column 10: Collapse rate XI

Column 11: Total mass XMTOT

Column 12: Total ang. momentum XJTOT

Column 13: Total potential energy XPTOT

Column 14: Total kinetic energy XKTOT

The figure shows the acceleration of core-collapse due to rotation (central density in code units vs. time). The black line represents a non-rotating, the red line a high initial rotating case (ωo=0.9). See also Fig. 3 of Fiestas et al. 2004.

-routine to generate the plot: dtime.pro

The figure shows the initial distribution function (King model) against angular momentum (curves of constant energy) for the model (6.0,0.3) See also Figs. 1 and 2 of Fiestas et al. 2004.

-routine to generate the plot: df.pro

The figure shows a contour map (on meridional plane) of the rotational velocity for a collapsed model of initial (6.0,0.9) at time t/trh=4.7. Distances are given in units of initial core radius, velocity in code units.

-routine to generate the plot: vrot.pro

Contour map of 1-d velocity dispersion (on meridional plane) for a collapsed model of initial (6.0,0.9) at time t/trh=4.7. Distances are given in units of initial core radius, velocity in code units.

-routine to generate the plot: vdisp.pro

This figure shows the time evolution of dynamical ellipticity for the model Wo=6 and different initial rotation parameters (See also Fig. 4 of Fiestas et al. 2004).

-routine to generate the plot: edynage.pro

- Cohn (1980), Astrophys. J. 242, p765.
- Einsel C.. & Spurzem R. (1999), MNRAS, 302, p81. Paper I
- Gebhardt K., Pryor C., O'Connell R.D., Williams T.B.,Hesser J.E. (2000), Astrophys. J. 119, p1268
- Goodman (1983), PhD Thesis, Princeton University
- Kim E., EInsel C., Lee H.M., Spurzem R., Lee M.G. (2002),MNRAS 334, p310.Paper II
- King I.R., Anderson J. (2001), in S. Deiters et al., (eds), Dynamics of Star Clusters and the Milky Way, ASP Conf. Ser. 228, p19