The fate of planetesimals formed at planetary gap edges

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Volume 648 (April 2021)

A&A, 648 (2021) A112

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Table 1

Parameters for the simulations in the parameter study.

Solar System

Run	Jupiter		Saturn		α	Ṁ₀
	M_p	Comp.	M_p	Comp.		(M_⊙ yr⁻¹)
#1 Nominal	90 M_⊕	H₂O, CO₂	30 M_⊕	H₂O, CO₂	10⁻²	10⁻⁷
#2 Nominal (–CO₂)	90	H₂O	30	H₂O	10⁻²	10⁻⁷
#3 M_p ↓	30	H₂O, CO₂	10	H₂O, CO₂	10⁻²	10⁻⁷
#4 M_p ↑	150	H₂O, CO₂	50	H₂O, CO₂	10⁻²	10⁻⁷
#5 α ↓	90	H₂O, CO₂	30	H₂O, CO₂	10⁻³	10⁻⁷
#6 Ṁ₀ ↓	90	H₂O	30	H₂, CO₂	10⁻²	10⁻⁸

HL Tau

Run	Planet 1		Planet 2		Planet 3		α	Ṁ₀
	M_p	Comp.	M_p	Comp.	M_p	Comp.		(M_⊙ yr⁻¹)

#7 Nominal	59.6 M_⊕	H₂O, CO₂	141.2 M_⊕	H₂O, CO₂	313.7 M_⊕	H₂O, CO₂	10⁻²	10⁻⁷
#8 α ↓	-//-	H₂O, CO₂	-//-	H₂O, CO₂	-//-	H₂O, CO₂, CO	10⁻³	10⁻⁷
#9 α ↓ (–CO)	-//-	H₂O, CO₂	-//-	H₂O, CO₂	-//-	H₂O, CO₂	10⁻³	10⁻⁷
#10 α ↓ (–CO, –CO₂)	-//-	H₂O	-//-	H₂O	-//-	H₂O	10⁻³	10⁻⁷
#11 Ṁ₀ ↓	-//-	H₂O, CO₂	-//-	H₂O, CO₂	-//-	H₂O, CO₂	10⁻²	10⁻⁸

Notes. Here, M_p denotes planetary mass and “comp.” refers to the volatile composition of the planetesimals initiated at the gap edge of the specified planet.

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