Run 5

T/Myr Ns Nb Nbs Ndd Mtot/Msun log(L/Lsun) Rh
0.0 12288 4096 0 0 10174.3281 6.12 5.43
503.5 11389 3767 4 7 7836.8936 4.44 6.79
1007.0 10393 3484 3 17 7027.7212 4.09 6.99
1510.5 9451 3186 6 21 6370.9482 4.13 7.30
2014.0 8465 2924 5 26 5740.3882 4.09 7.31
2517.5 7616 2673 5 28 5228.5249 3.68 7.31
3021.0 6751 2434 8 31 4740.2134 3.60 7.45
3524.5 6001 2212 6 33 4322.3867 3.50 7.30
4028.0 5322 2031 5 36 3934.1465 4.02 7.23
4531.5 4624 1817 2 35 3518.9121 3.55 7.23
5035.0 3979 1649 2 36 3153.7173 3.46 7.32
5538.5 3407 1474 3 38 2807.9978 3.47 7.46
6042.0 2893 1321 2 32 2487.6475 3.52 7.27
6545.5 2463 1181 4 30 2219.5605 3.58 7.40
7049.1 2037 1046 4 29 1931.7041 3.62 7.66

Colour Magnitude diagrams

Colour-magnitude diagrams for the KyotoII experiment. Main-sequence stars (black points), blue stragglers (filled blue circles), sub-giants and giants (filled red circles), naked helium stars (cyan points), and white dwarfs (magenta points) are depicted. Binary stars are denoted by overlapping filled circles of colours appropriate to the stellar type of the components, with main-sequence binary components shown as green. The bolometric corrections computed by Kurucz (1992, IAU Symp. 149, p.225) from synthetic stellar spectra have been used to convert theoretical stellar quantities to observed colours. These corrections are strictly not valid for WDs and extremely cool giants.

1 Gyr; 3 Gyr; 5 Gyr; 7 Gyr


Note: there is some doubt about the implementation of the tide in this run.