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Table 3

Parameters of the circumstellar disks and the migration scenarios considered in the 18 formation simulations for V1298 Tau’s planets b and e, and the resulting accretion of heavy elements of each scenario.

Id. Disk V1298 Tau b V1298 Tau e
Mdisk (M⊙) Σ0 (g cm−3) Mdust (M⊕) Initial seed (au) Δa1 (au) Δa2 (au) Accretedmass (M⊕) Initial seed (au) Δa1 (au) Δa2 (au) Accreted mass (M⊕)
1 0.06 42 205 11 −6.4 −4.3 22 50 −29.6 −19.8 54
2 0.06 42 205 10 −5.8 −3.9 19 30 −17.6 −11.8 46
3 0.06 42 205 10 −5.8 −3.9 18 20 −11.6 −7.8 26
4 0.06 42 205 11 −6.4 −4.3 21 22 −12.8 −8.6 28
5 0.12 80 390 6 −3.4 −2.3 15 50 −29.6 −19.8 139
6 0.12 80 390 6 −3.4 −2.3 13 15 −8.6 −5.8 52
7 0.12 80 390 9 −5.2 −3.5 30 50 −29.6 −19.8 132
8 0.12 80 390 9 −5.2 −3.5 36 12.5 −7.1 −4.8 11
9 0.12 80 390 7.5 −4.3 −2.9 20 50 −29.6 −19.8 129
10 0.12 80 390 7.5 −4.3 −2.9 19 15 −8.6 −5.8 41
11 0.12 80 390 7.5 −4.3 −2.9 20 12.5 −7.1 −4.8 25
12 0.12 80 390 7.5 −4.3 −2.9 19 13 −7.4 −5.0 28
13 0.18 120 585 5 −2.8 −1.9 7 50 −29.6 −19.8 250
14 0.18 120 585 10 −5.8 −3.9 48 50 −29.6 −19.8 233
15 0.18 120 585 7.5 −4.3 −2.9 26 50 −29.6 −19.8 234
16 0.18 120 585 7 −4 −2.7 23 50 −29.6 −19.8 245
17 0.18 120 585 7 −4 −2.7 23 12.5 −7.1 −4.8 42
18 0.18 120 585 7 −4 −2.7 23 11 −6.2 −4.2 28

Notes. The rows highlighted in blue identify the simulations consistent with the LMZe scenario in Table 2. The row highlighted in red is the simulation consistent with the HMZe scenario, while the row highlighted in yellow identifies the simulation consistent with the HMZe scenario when assuming a second process assists in increasing the metallicity of planet e.

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