How drifting and evaporating pebbles shape giant planets - I. Heavy element content and atmospheric C/O

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Volume 654 (October 2021)

A&A, 654 (2021) A71

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This article has an erratum: [https://doi.org/10.1051/0004-6361/202141096e]

Table 2

Condensation temperatures and volume mixing ratios of the chemical species.

Species (Y)	T_cond (K)	v_{Y, no C}	v_{Y, with C}
CO	20	0.45 × C/H	0.45 × C/H
N₂	20	0.9 × N/H	see v_{Y, no C}
CH₄	30	0.45 × C/H	0.25 × C/H
CO₂	70	0.1 × C/H	0.1 × C/H
NH₃	90	0.1 × N/H	see v_{Y, no C}
H₂S	150	0.1 × S/H	see v_{Y, no C}
H₂O	150	O/H - (3 × MgSiO₃/H + 4 × Mg₂SiO₄/H + CO/H
		+ 2 × CO₂/H + 3 × Fe₂O₃/H + 4 × Fe₃O₄/H + VO/H
		+ TiO/H + 3 × Al₂O₃ + 8 × NaAlSi₃O₈ + 8 × KAlSi₃O₈)	see v_{Y, no C}
Fe₃O₄	371	(1/6) × (Fe/H - 0.9 × S/H)	see v_{Y, no C}
C (carbon grains)	631	0	0.2 × C/H
FeS	704	0.9 × S/H	see v_{Y, no C}
NaAlSi₃O₈	958	Na/H	see v_{Y, no C}
KAlSi₃O₈	1006	K/H	see v_{Y, no C}
Mg₂SiO₄	1354	Mg/H - (Si/H - 3 × K/H - 3 × Na/H)	see v_{Y, no C}
Fe₂O₃	1357	0.25 × (Fe/H - 0.9 × S/H)	see v_{Y, no C}
VO	1423	V/H	see v_{Y, no C}
MgSiO₃	1500	Mg/H - 2 × (Mg/H - (Si/H - 3 × K/H - 3 × Na/H))	see v_{Y, no C}
Al₂O₃	1653	0.5×(Al/H - (K/H + Na/H))	see v_{Y, no C}
TiO	2000	Ti/H	see v_{Y, no C}

Notes. Condensation temperatures for molecules are taken from Lodders (2003). For Fe₂ O₃ the condensation temperature for pure iron is adopted (Lodders 2003). Volume mixing ratios v_Y (i.e., by number) are adopted for the species as a function of disk elemental abundances (see, e.g., Madhusudhan et al. 2014). We expand hereon the different mixing ratios from Bitsch & Battistini (2020). Results in this work apply the model without pure carbon grains. A comparison with a model that includes carbon grains can be found in Appendix D.

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