Table B.2
Comparison of existing GI population syntheses.
| Publication | Forgan & Rice (2013) | Müller et al. (2018) | Nayakshin (2015a) | Nayakshin (2015b) | Nayakshin & Fletcher (2015) | Nayakshin (2016) | Humphries et al. (2019) |
|---|---|---|---|---|---|---|---|
| Title | Towards a population synthesis model of objects formed by self-gravitating disc fragmentation and tidal downsizing | On the Diversity in Mass and Orbital Radius of Giant Planets Formed via Disk Instability | Tidal Downsizing model -1. Numerical methods: saving giant planets from tidal disruptions | Tidal Downsizing model. II. Planet- metallicity correlations | Tidal downsizing model - III. planets from subearths to brown dwarfs: Structure and metallicity preferences | Tidal Downsizing model - IV. Destructive feedback in planets | Constraining the initial planetary population in the gravitational instability model |
| Viscous a | 0.005 | 0.005 | 0.01 | [0.001..0.01] | 0.005 | [O.OO5..O.O5] | 0.005 |
| Glɑ | Gammie (2001) | Kratter et al. (2008) | – |  |
 |
 |
0.12 |
| Type Imig | tI.FR | Baruteau et al. (2011) |  |
[1..10] × tI,N | [0.5..2] × tI,n | [1..4] × tI,N | 0.8 × tI,n |
| Type II mig | tII,FR | viscous1 | impulse approx. | impulse approx. | impulse approx. | impulse approx. |  |
| Gap opening | Armitage & Bonnell (2002)0 | various1 | Crida et al. (2006) | Crida et al. (2006) | Crida et al. (2006) | Crida et al. (2006) | Crida et al. (2006)2 |
| Gas accretion | — | Galvani & Mayer (2014) | — | — | — | — | — |
| Pebble accretion | — | — | ✓ | ✓ | ✓ | ✓ | — |
| # fragments | several3 | 1 | 1 | 1 | 1 | 1 | 1 |
| Condition for frag. | Forgan & Rice (2011) | —4 | —5 | —5 | 5 | —5 | —5 |
| 2nd collapse | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ |
| Initial fragment location | randomly in unstable region | [80..120] au | 100au | [60..120] au | [70..105] au | [70..105] au | [40..300] au |
| Tidal downsizing | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ |
| Thermal bath disruption | — | — | ✓ | ✓ | ✓ | ✓ | ✓ |
| Initial stellar mass | [0.8..1.2] M⊙ | 0.6, 1.0, 1.4, 2.4 msun | 1 M⊙ | 1 M⊙ | 1 M⊙ | 1 M⊙ | 1 M⊙ |
| Initial disc mass | [0.125..0.375] M⊙ | 0.18, 0.3, 0.42, 0.72 M⊙ | 0.12 M⊙ | [0.05..0.2] M⊙ | [0.075..0.15] M⊙ | [0.075..0.2]M⊙ | [0.1..0.3] M⊙ |
| Initial q = Md/M* | constant | 0.3 | 0.12 | 0.05-0.2 | 0.075-0.15 | 0.075-0.2 | 0.1-0.3 |
| Initial disc radius | [50..100] au | ≈ 120 au | 120au | 100 au | 100 au | 100 au | 80-300 au |
| Initial surface density profile | —1 | —1/2,-1.-3/2 | —1 | —1 | —1 | —1 | —1 |
| Photoevaoration | Owen et al. (2010) | — | — | UV and X-ray6 | 6 and7 | 6 and7 | — |
| Initial fragment mass | Forgan & Rice (2011) | 0.5 M♃ to 16M, | 1 M♃ or 5 M♃ | 0.5, 0.7, 1 or 2 M♃ | [0.333.,16] M♃ | [0.333..8] M, | 1.3. 5.7 M♃ |
| Clump structure | FC8 | varied | FC8 | FC8 | FC8 | FC8 | Vazan & Helled (2012) |
| Clump contraction | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ |
| Grain growth | ✓ | — | ✓ | ✓ | ✓ | ✓ | — |
| Grain sedimentation | ✓ | — | ✓ | ✓ | ✓ | ✓ | — |
| Core formation and growth | ✓ | — | ✓ | ✓ | ✓ | ✓ | — |
| N-body interaction | —/(✓)9 | — | — | — | — | — | — |
Notes. If ranges are given in brackets, it means the corresponding values are sampled in a Monte Carlo approach from the given interval. The updated Forgan & Rice mode. ’Towards a population synthesi‘s model of self-gravitating disc fragmentation and tidal downsizing II: the effect of fragment-fragment interactions’, is not included in a separate row. However, the differences are explained. See text for further explanations.
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