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Dust Formation in AGN Winds

• Authors: Arkaprabha Sarangi, Eli Dwek, and Demos Kazanas

2019 The Astrophysical Journal 885 126.

• Provider: AAS Journals

Caption: Figure 10.

Left panel: the color map shows the total number density of dust grains composed of sizes ranging between 10 and ∼200 Å in polar (r, θ) coordinates. The black lines in the figure represent the parabolic flow lines with various starting/launch radii on the accretion disk, r0. As seen in the figure, for each radius the number density of grains increases at higher inclinations, i.e., close to the plane of the accretion disk at θ ∼ 90°. The figure shows that the dust-forming region has a toroidal morphology. The three horizontal lines correspond to the inclination angles, for which the dust densities are shown in the right panel in the same color code. Right panel: the number density of dust grains is presented as a function of radial distance r for inclination angles θ = 30°, 75°, and 85°. The presence of a dust toroidal region at high inclination angles is further visible in the figure.