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Home All issues Volume 497 / No 1 (April I 2009) A&A, 497 1 (2009) 255-264 Full HTML
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Table 1:

Parameters and results of the first collision sequence studied in this paper. Time t in Myr, masses are in solar units. The final row gives the age at which our evolution calculations stopped and the mass of the collision product at the end of the evolution (assumed black hole mass).
N t $M_{1,N\mbox{-}{\rm body}}^{a}$ $M_{1,{\rm mix}}^{a}$ $M_{1,{\rm MMS}}^{a}$ M2a $M_{\rm merger}^{a}$
1 0.22577 92.4 90.9 90.9 79.4 154.3
2 0.22782 171.8 154.3 152.8 85.3 217.1
3 0.23702 257.1 216.7 213.6 7.7 223.3
4 0.31217 264.8 219.8 215.3 77.8 274.4
5 0.40122 342.6 268.2 261.6 13.8 279.7
6 0.43480 356.4 277.2 268.0 71.9 327.1
7 0.43480 428.3 327.1 315.1 79.4 382.2
8 0.74123 507.7 348.2   30.1 371.8
9 0.83549 537.7 360.2   66.7 406.7
10 0.90575 604.5 397.3   1.2 398.5
11 1.29919 605.7 353.5   98.2 415.2
12 1.33450 703.9 411.0   24.2 430.8
13 1.42468 728.0 417.6   8.9 425.7
14 1.50261 736.9 409.0   2.2 411.2
15 1.60190 739.1 216.7   60.2 256.5
16 1.63186 799.4 221.0   9.2 228.9
17 1.68112 808.5 186.0   81.1 237.1
18 1.75684 889.6 177.3   40.9 205.5
19 1.90688 930.5 193.6   31.6 216.3
20 2.07245 961.9 129.9   2.6 132.2
21 2.59778 963.1 47.6   55.2 88.6
22 3.10786 1012.7 40.9   75.4b 110.1
  3.72835 1118.9 13.9      
a
The primary mass according to the N-body code $M_{1,N\mbox{-}{\rm body}}$ and according to our fully mixed models $M_{1,{\rm mix}}$, the mass of the secondary M2 and the mass of the fully mixed remnant after the collision $M_{\rm merger}$. The mass $M_{1,{\rm MMS}}$ according to the MMAMS models we were able to calculate is given for comparison.
b
See text.

Source LaTeX | All tables | In the text

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