English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

(Abridged) Infrared high-resolution imaging and interferometry have shownthat the dust distribution is frequently elongated along the polar direction ofan AGN. To explain these findings, we developed a model scenario for the inner~30 pc of an AGN. We assume a rotating thick gas disk between about one and tenparsec. External gas accretion adds mass and injects energy via gas compressioninto this gas disk and drives turbulence. Our disks are assumed to be stronglymagnetized via equipartition between the turbulent gas pressure and the energydensity of the magnetic field. In a second step, we built three dimensionaldensity cubes based on the analytical model, illuminated them with a centralsource, and made radiative transfer calculations. In a third step, wecalculated MIR visibility amplitudes and compared them to availableinterferometric observations. We show that magnetocentrifugal winds startingfrom a thin and thick gas disk are viable in active galaxy centers. Once thewind is launched, it is responsible for the transport of angular momentum andthe gas disk can become thin. The outflow scenario can account for theelongated dust structures, outer edges of the thin maser disks, and molecularoutflows observed in local AGN. The models reproduce the observed terminal windvelocities, the scatter of the MIR/intrinsic X-ray correlation, and pointsource fractions. An application of the model to the Circinus Galaxy and NGC1068 shows that the IR SED, available MIR interferometric observations, andoptical polarization can be reproduced in a satisfactory way, provided that (i)a puff-up at the inner edge of the thin disk is present and (ii) a local screenwith an optical depth of tau_V 20 in form of a local gas filament and/or a warpof the thick disk hide a significant fraction of both nuclei.

Thick turbulent gas disks with magnetocentrifugal winds in active galactic nuclei - Model infrared emission and optical polarization