Table 1
Summary of our models at the onset of the runaway accretion phase (Mtot = 58 M⊕) and the accretion parameters.
| MZ [M⊕ ] | Sph [kb ∕mu ] | R[RJ] | Ṁmax [M⊕ yr−1] | χ | Zacc | Lf [L⊙] | |
|---|---|---|---|---|---|---|---|
| Hot_compact_Z | 23 | 8.1 | 1.2 | 10−2 | 1 | 0.04 | 5 × 10−4 |
| Hot_extended_Z | 16 | 6.5 | 1.3 | 10−2 | 1 |  |
2 × 10−4 |
| Cold_extended_Z | 16 | 6.5 | 1.3 | 10−4 | 0 |  |
1 × 10−6 |
| Cold_high_Z | 28 | 5.0 | 1.0 | 10−4 | 0 |  |
1 × 10−6 |
Notes. The columns are the total heavy-element mass MZ, photospheric entropy Sph per baryon, planetary radius in units of Jupiter’s radius, max. accretion rate Ṁmax, shock temperature parameter χ, the heavy-element fraction of the accreted material Zacc, and the post-formation luminosity Lf. We note that the difference in entropy between models is mainly due to the composition. The accretion parameters are chosen such that Hot-compact_Z & Hot_extended_Z create hot-start planets, while Cold_extended_Z Cold_high_Z create cold proto-Jupiters. The composition of the accreted material is either kept constant (Hot_compact_Z), or is changing as Jupiter grows. This creates a composition profile similar to that of Vazan et al. (2018) (Hot_extended_Z & Cold_extended_Z) or with a much larger fraction of heavy elements in the envelope (Cold-high_Z).
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