Interior dynamics of envelopes around disk-embedded planets

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Volume 707 (March 2026)

A&A, 707 (2026) A26

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Table 1

Parameters of hydrodynamical simulations.

	m	β	Ṁ	N_r	`xorder`	t_end	r_in
Fiducial runs	0.1	0.01, 0.1, 1, 10, 30, 100, 300, 1000, 10000	10 M_⊕/Myr	256	2	50	10 R_p/H
	0.2	10, 30, 100, 300, 1000	10 M_⊕/Myr	256	2	50	10 R_p/H
	0.3	10, 30, 100, 300, 1000	10 M_⊕/Myr	256	2	50	10 R_p/H
Low luminosity runs	0.1	10, 100, 1000	1 M_⊕/Myr	256	2	50	10 R_p/H
	0.2	10, 100, 1000	1 M_⊕/Myr	256	2	50	10 R_p/H
	0.3	10, 100, 1000	1 M_⊕/Myr	256	2	50	10 R_p/H
High luminosity runs	0.1	10, 100, 1000	100 M_⊕/Myr	256	2	50	10 R_p/H
	0.2	10, 100, 1000	100 M_⊕/Myr	256	2	50	10 R_p/H
	0.3	10, 100, 1000	100 M_⊕/Myr	256	2	50	10 R_p/H
Convergence tests	0.1	1, 1000	10 M_⊕/Myr	168	2, 3	10	10 R_p/H
	0.1	1, 1000	10 M_⊕/Myr	196	2, 3	10	10 R_p/H
	0.1	1, 10, 100, 1000	10 M_⊕/Myr	256	3	10	10 R_p/H
	0.1	1, 1000	10 M_⊕/Myr	256	2	10	5 R_p/H

Notes. The following columns give the dimensionless thermal mass, the dimensionless cooling time, the pebble accretion rate, the radial resolution, the method for spatial reconstruction, the calculation time, and the size of the inner boundary.

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