Table 2
Variation in final core masses for different pebble sizes, disk conditions, and accretion rates.
| Parameter | Variation | Final core masses (M⊕) | |
|---|---|---|---|
| – | – | 0.42 | 0.59 |
| Ri | 0.01 (m) | 0.31 | 0.59 |
| Ri | 1 (m) | 0.52 | 0.58 |
| EOS | QEOS (1) | 0.42 | 0.59 |
| Ṁacc | 10−4 (M⊕ yr−1) | 0.41 | 0.55 |
| Ṁacc | 10−6 (M⊕ yr−1) | 0.42 | 0.65 |
| dplanet | 10 (AU) | 0.40 | 0.60 |
| dplanet | 1 (AU) | 0.41 | 0.54 |
| dplanet | 0.5 (AU) | 0.33 | 0.48 |
| dplanet | 0.2 (AU) | 0.23 | 0.37 |
 |
40 (g mol−1) | 0.42 | 0.66 |
 |
18 (g mol−1) | 0.43 | 0.97 |
 |
10 (g mol−1) | 0.44 | 1.49 |
 |
1.4 | 0.42 | 0.66 |
 |
1.1 | 0.42 | 0.57 |
Notes. The final column (left and right) shows the core masses at which either pebbles are fully evaporated (mixing scenario; left) or all ablated material can be absorbed by the envelope as vapor (rainout scenario; right). The standard model parameters are given in Table 1.
References. (1) Vazan et al. (2013).
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