A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201117910e]

Table 6

Parameters for the moving star simulations.

Label	description	Ṁ	M_dust/M_gas	v_⋆	n_ISM	T_ISM	Physical space	Basic grid	R₀^a	R_s^b
		(M_⊙ yr^-1)	(%)	(km s^-1)	(cm^-3)	(K)	(pc)		(pc)	(pc)

A	basic model^c	10^-6	1	25	2	1	1.5 × 1	120 × 80	0.26 ± 0.01	0.35
B	high Ṁ	10^-5	1	25	2	1	2 × 2	160 × 160	0.59 ± 0.03	0.73
C	low Ṁ	10^-7	1	25	2	1	2 × 1	160 × 80	0.090 ± 0.001	0.10
D	low dust	10^-6	0.1	25	2	1	2 × 1	160 × 80	0.33 ± 0.03	0.33
E	high v_⋆	10^-6	1	75	2	1	1.5 × 1	120 × 80	0.11 ± 0.02	0.13
F	low n_ISM	10^-6	1	25	0.2	1	3 × 2	240 × 160	0.76 ± 0.08	0.92
G	warm ISM	10^-6	1	25	2	8 000	2 × 2	160 × 80	0.31 ± 0.06	0.45

Notes.

^(a)

Estimated. Large-scale instabilities make R₀ (contact discontinuity) a time-dependent property. In particular, for simulations E and G the mixing is very efficient, eliminating in effect the contact discontinuity altogether.

^(b)

R_s, the location of the forward shock of the shocked gas region, where the ISM transition from unshocked to shocked gas can be more accurately measured.

^(c)

v_w = 15 km s^-1 for all models.

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