The role of thermal instability in accretion outbursts in high-mass stars

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Volume 692 (December 2024)

A&A, 692 (2024) A256

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Table 3.

Main properties of outbursting HMYSOs.

Object	Mass	Radius	Burst duration	Rise time	Ṁ_peak	Accreted mass	Multiple
	[M_⊙]	[R_⊙]	[yr]	[yr]	[M_⊙ yr⁻¹]	[M_J]	bursts
M17 MIR ^(§)	5.4	10.1 − 34.1	9 − 20	< 1	5 × 10⁻³, 2 × 10⁻³	∼30(×2)	Yes
NGC 6334I MM1 ^( * )	6.7	2.6 − 20	> 8	0.62 $_{- 0.14}^{+ 0.14}$ $^{+0.14}_{-0.14}$	2.3 × 10⁻³	0.325 $_{- 0.094}^{+ 0.126}$ $^{+0.126}_{-0.094}$	No
G358.93−0.03 MM1 ^( ‡ )	9.7 $_{- 0.6}^{+ 0.3}$ $^{+0.3}_{-0.6}$	3.9 $_{- 0.2}^{+ 0.1}$ $^{+0.1}_{-0.2}$	0.75	0.16 $_{- 0.01}^{+ 0.01}$ $^{+0.01}_{-0.01}$	$1 . 8_{- 1.1}^{+ 1.2} \times 10^{- 3}$ $1.8^{+1.2}_{-1.1}\times10^{-3}$	0.566	No
V723 Car ^(¶)	10	18 − 58	5	4	–	–	No?
S255IR NIRS 3 ^( † )	20	10	2 − 2.5	0.4	5 × 10⁻³	2	Yes ^($)
G323.46−0.08 ^( * *)	23	–	8.4	1.4	0.8 × 10⁻³
W51 IRS2 ^(⋄)	40–60 ^( ▿ )	–	< 1	≪1	–	∼260(0.25 M_⊙)	No

Notes. ^( † )Caratti o Garatti et al. (2017), ^( * )Hunter et al. (2017, 2021), ^( ‡ )Stecklum et al. (2021), ^(¶)Tapia et al. (2015), ^( * *)Proven-Adzri et al. (2019), Wolf et al. (2024), ^(§)Chen et al. (2021), ^(⋄)Zhang et al. (2022), ^( ▿ )Zapata et al. (2009). ^($)Based on sparse photometric observations of Fedriani et al. (2023).

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