Non-stoichiometric amorphous magnesium-iron silicates in circumstellar dust shells - Dust growth in outflows from supergiants

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Table 6

Properties of dust models with accelerated velocity and initial velocity v₀ = 2 km s⁻¹.

			Mass-loss rate Ṁ_i and composition						Temperature T_i

Object	χ²	τ_10μm	Sil	Mg#	Dirty	f_inc	Cor	Iron	Sil	Dirty	Cor	Iron	τ_SiO	g/d
μ Cep	0.024	0.0140	2.47	0.61	r		0.190	0.309	910		1400	490	0.31	2451
RW Cyg	0.095	0.0361	4.18	0.48	r		0.623	1.055	938		1400	335	0.99	1202
W Per	0.101	0.0337	2.87	0.56	r		0.260	0.399	614		1400	343	0.60	631
RS Per	0.077	0.0192	1.92	0.47	r		0.326	0.363	923		1400	424	0.33	1302
α Ori	0.109	0.0035	0.125	0.62	r		0.0324	r	981		1400		0.21	691
α Sco	0.034	0.0017	0.0886	0.80	r		0.0153	0.0044	816		1400	741	0.10	705
S Per	0.168	0.0558	2.82	0.77	1.82	0.278	0.909	0.101	854	608	1400	432	2.41	1050
PZ Cas	0.117	0.0612	51.2	0.63	4.63	0.372	0.683	0.706	402	400	1400	307	1.98	451
VX Sgr	0.071	0.0484	7.82	0.79	5.62	0.249	1.021	1.905	827	606	1400	691	2.83	2291

Notes. The dust mass-loss rates are in units of 10⁻⁹ M_⊙ yr⁻¹ and the temperatures in Kelvin. Species rejected by the optimisation are marked by “r”.

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