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The role of infrared radiation pressure in shaping dusty winds in AGN

The role of infrared radiation pressure in shaping dusty winds in AGN
The role of infrared radiation pressure in shaping dusty winds in AGN
The detection of dusty winds dominating the infrared emission of AGN on parsec scales has revealed the limitations of traditional radiative transfer models based on a toroidal distribution of dusty gas. A new, more complex, dynamical structure is emerging and the physical origin of such dusty winds has to be critically assessed. We present a semi-analytical model to test the hypothesis of radiatively accelerated dusty winds launched by the AGN and by the heated dust itself. The model consists of an AGN and an infrared radiating dusty disk, the latter being the primary mass reservoir for the outflow. We calculate the trajectories of dusty gas clumps in this environment, accounting for both gravity and the AGN radiation as well as the re-radiation by the hot dusty gas clouds themselves. We find that the morphology consists of a disk of material that orbits with sub-Keplerian velocities and a hyperboloid polar wind launched at the inner edge of the dusty disk. This is consistent with high-angular resolution infrared and sub-mm observations of some local Seyfert AGN. The strength of the wind and its orientation depend on the Eddington ratio and the column density of the dusty clumps, which is in agreement with propose
0004-637X
Venanzi, Marta
3f4e3e23-62a1-4654-8860-25a3228d7470
Hoenig, Sebastian
be0bb8bc-bdac-4442-8edc-f735834f3917
Williamson, David
140b2434-b216-4237-8a78-9950b01319b5
Venanzi, Marta
3f4e3e23-62a1-4654-8860-25a3228d7470
Hoenig, Sebastian
be0bb8bc-bdac-4442-8edc-f735834f3917
Williamson, David
140b2434-b216-4237-8a78-9950b01319b5

Venanzi, Marta, Hoenig, Sebastian and Williamson, David (2020) The role of infrared radiation pressure in shaping dusty winds in AGN. Astrophysical Journal. (In Press)

Record type: Article

Abstract

The detection of dusty winds dominating the infrared emission of AGN on parsec scales has revealed the limitations of traditional radiative transfer models based on a toroidal distribution of dusty gas. A new, more complex, dynamical structure is emerging and the physical origin of such dusty winds has to be critically assessed. We present a semi-analytical model to test the hypothesis of radiatively accelerated dusty winds launched by the AGN and by the heated dust itself. The model consists of an AGN and an infrared radiating dusty disk, the latter being the primary mass reservoir for the outflow. We calculate the trajectories of dusty gas clumps in this environment, accounting for both gravity and the AGN radiation as well as the re-radiation by the hot dusty gas clouds themselves. We find that the morphology consists of a disk of material that orbits with sub-Keplerian velocities and a hyperboloid polar wind launched at the inner edge of the dusty disk. This is consistent with high-angular resolution infrared and sub-mm observations of some local Seyfert AGN. The strength of the wind and its orientation depend on the Eddington ratio and the column density of the dusty clumps, which is in agreement with propose

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The role of infrared radiation pressure in shaping dusty winds in AGN - Accepted Manuscript
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Accepted/In Press date: 21 July 2020
Additional Information: arxiv is am

Identifiers

Local EPrints ID: 444482
URI: http://eprints.soton.ac.uk/id/eprint/444482
ISSN: 0004-637X
PURE UUID: 61c5f0f9-49c7-481f-9587-f333597370bc
ORCID for David Williamson: ORCID iD orcid.org/0000-0002-5168-7979

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Date deposited: 21 Oct 2020 16:31
Last modified: 18 Feb 2021 17:30

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Contributors

Author: Marta Venanzi

University divisions

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