Table 1
Results of the two sets of simulations, with and without planetesimal fragmentation (PF).
| # |  km |
 km |
 km |
 km |
||||||||||||
|
|
||||||||||||||||
| Without PF | With PF | Without PF | With PF | Without PF | With PF | Without PF | With PF | |||||||||
| M C | t | M C | t | M C | t | M C | t | M C | t | M C | t | M C | t | M C | t | |
| (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | (M⊕) | (Myr) | |
|
|
||||||||||||||||
| 2 | 23.10 | 4.41 | 0.04 | 6.00 | 5.84 | 6.00 | 0.04 | 6.00 | 0.35 | 6.00 | 0.06 | 6.00 | 0.11 | 6.00 | 0.11 | 6.00 |
| 4 | 32.23 | 0.39 | 0.09 | 6.00 | 21.37 | 2.99 | 0.08 | 6.00 | 9.17 | 6.00 | 0.18 | 6.00 | 0.56 | 6.00 | 0.52 | 6.00 |
| 6 | 35.25 | 0.17 | 0.20 | 6.00 | 27.55 | 0.92 | 0.12 | 6.00 | 21.55 | 3.27 | 0.39 | 6.00 | 2.13 | 6.00 | 1.34 | 6.00 |
| 8 | (...) | (...) | 0.45 | 6.00 | 35.73 | 0.33 | 0.15 | 6.00 | 27.77 | 1.64 | 0.67 | 6.00 | 14.99 | 6.00 | 3.58 | 6.00 |
| 10 | (...) | (...) | 0.77 | 6.00 | 45.78 | 0.15 | 0.18 | 6.00 | 32.64 | 0.99 | 1.00 | 6.00 | 25.06 | 4.07 | 7.13 | 6.00 |
Notes. The first column corresponds to the disk mass. A value of # means
that we consider a disk # times more massive than the minimum mass solar nebula (MMSN)
of Hayashi (1981). MC
represents the core mass when the planet achieves the critical mass and
t
represents the time at which this occurs. Simulations stopped at t = 6 Myr, so that in
this case MC represents the core mass at this
time. For km and for disks 8 and 10
times more massive than the MMSN, planetesimal accretion rates become so high that
models do not converge when planetesimal fragmentation is not considered.
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