Initial and boundary conditions
Our aim is to choose a model displaying an interesting interplay
of stellar and dynamical evolution, and doable by as many groups as possible.
Useful guidance is offered by Hurley et al, MNRAS, 2001, 323,
630, whose model with N_{s} = N_{b} = 5000
took 1 month on a GRAPE 4.
Specification
Structure

King, W_{0}=5

no initial mass segregation
Boundary condition

r_{t } = 27.9pc (initially)

tidal cutoff
Single stars

N_{s} = 12288

IMF of single stars: KTG3*, 0.1M<m< 100M, where M is 1 solar mass
*Kroupa, Tout & Gilmore, MNRAS, 1993, 262, 545; eq.(14) & Table
10 with alpha_{1}=1.3
Primordial binaries

N_{b} = 4096

f(e) = 2e

total binary mass: KTG1 (see Hurley et al, eq.(1)), range [0.2M,200M]

mass ratio q<1, uniform in range giving masses in [0.1M, 100M]

a: uniform in log a in a range such that a(1e) > 2(R_{1}+R_{2})
and energy exceeds 10kT. Here radii are fromEggleton, Fitchett &
Tout, 1989, ApJ, 347, 998
Stellar evolution
Discussion (under construction)
N = 20480, f_{b } = 0.25m, N_{s} + N_{b}
= 16K
For the initial data generated for this project, the total mass is
approximately 10174M. For a pointmass galaxy, galactocentric
distance R_{G}=8.5kpc, circular velocity v_{G }= 220km/s,
r_{t } = 27.9pc approximately.
=> M ± 813000MM
=> lifetime ± 7.6Gyr (V&H)
(=>30% in [10kT,100kT])
Possible sources:
Single stars: Eggleton, Fitchett & Tout, 1989, ApJ, 347,
998
Binary stars: Tout, Aarseth, Pols, 1997, MNRAS, 291, 732
Portegies Zwart, McMillan, Hut, Makino, 2001,
MNRAS, 321, 199 (and references therein)