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

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Table 4

Radii outside which the dust distributions are optically thin for all considered wavelengths.

Mass	Sphere	Spiral	Disc
(M_⊙)	radius (au)	radius (au)	radius (au)
	at τ_ν ~ 1	at τ_ν ~ 1	at τ_ν ~ 1
10⁻⁴	655	5000	4590
10⁻⁵	73	4990	2650
10⁻⁶	8	4940	505
10⁻⁷	<5	4410	55
10⁻⁸	<5	2170	6

Notes. Maximum optical thickness is obtained with our extinction coefficients at λ = 0.38 μm. For the spiral and disc models, an inclination angle of 90° is adopted (i.e. edge-on) and no spherical component is included.

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