Episodic accretion in high-mass star formation: An analysis of thermal instability for axially symmetric disks

Open Access

Table 1.

Main properties of the models.

Model	Parameters
TI_1 (fiducial)	M_* = 10 M_⊙
	$M_{disk} (r < 10 au) = 0.1 M_{⊙}$ $M_{\mathrm{disk}}{{(r < 10\,\rm{au})}} = 0.1\,{\text{ M}_{\odot}}$
	α_c/α_h = 0.05/0.5
	r_in = 0.08 au
	Ṁ_dep = 8 × 10⁻⁴ M_⊙ yr⁻¹
	r_dep = 3.7 au


Model	Difference from fiducial

TI_2	r_dep = 10 au
TI_3	Ṁ_dep = 3 × 10⁻⁴ M_⊙ yr⁻¹
TI_4	Ṁ_dep = 5 × 10⁻³ M_⊙ yr⁻¹
TI_5	M_disk = 2.0 M_⊙; Ṁ_dep = 3 × 10⁻⁴ M_⊙ yr⁻¹
TI_6	r_in = 0.04 au
TI_7	r_in = 0.12 au
TI_8	r_in = 0.16 au
TI_9	α_h = 0.1
TI_10	α_c = 0.2
TI_11	x2 resolution
TI_12	x4 resolution
TI_13	x8 resolution
TI_14	M_* = 5 M_⊙; r_in = 0.04 au
TI_15	M_* = 20 M_⊙; r_in = 0.12 au

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