How to disentangle geometry and mass-loss rate from AGB-star spectral energy distributions - The case of EP Aquarii

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Volume 642 (October 2020)

A&A, 642 (2020) A142

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Table 5

Fitted dust BB-temperatures and wavelengths, λ_BB, that correspond to the frequency of the peak of the BB-function B_ν(λ, T_dust) for spherical models, and edge-on spirals and discs.

Mass	Model	T_dust	λ_BB	R_dust
(M_⊙)		(K)	(μm)	(au)
10⁻⁴	Sphere	227	22	152
	Spiral	133	38	573
	Disc	50	102	6590^(a)
10⁻⁵	Sphere	287	18	85
	Spiral	629	8	12^(b)
	Disc	120	43	747
10⁻⁶	Sphere	287	18	85
	Spiral	411	12	34
	Disc	340	15	55
10⁻⁷	Sphere	287	18	85
	Spiral	411	12	34
	Disc	298	17	80^(b)
10⁻⁸	Sphere	287	18	85
	Spiral	293	17	80
	Disc	519	10	19^(b)

Notes. ^(a) Dust BB-radius may appear as >5000 au even thoughthere is no dust there since the dust we do see is colder than it would have been in an optically thin model. ^(b) In these examples the BB-fit to the simulated SED was complicated by the presence of strong silicate features.

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