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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 1.

Left panel: schematic representation of the helical outflow of the gas from the accretion disk, controlled by the magnetic field of the central BH. Assuming azimuthal symmetry, the projection of the motion of the wind in the x-z plane is shown in blue. The arrowheads indicate the direction of flow. For a more accurate presentation of this figure, we refer to Fukumura et al. (2018a) (Figure 3). Right panel: the projection of the accretion disk (AD) is shown along with the outflowing winds (in blue) in the upper hemisphere. The motion of the outflows along this plane can be represented by parabolic equations of motion. The luminosity of the system is attributed to a central X-ray UV source. The dotted line (in red) represents the sublimation radius and the dust-free zone.

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