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

Self-gravitating accretion discs have only been studied in a few nearbyobjects using maser spots at the parsec-scale. We find a new spectral windowfor observing the self-gravitating accretion disc in super-Eddington accretingActive Galactic Nuclei (AGNs). This window is determined by calculating theoutermost radius (rsg) of a non self-gravitating disc and the correspondingemission wavelength (lsg) as a function of various disc parameters. We findthat lsg reaches ~ 4000 AA for alpha=0.1, when Mdot > 70 (M_BH / 10^7 M_Sun)^-1L_Edd/c^2 (where alpha, Mdot, M_BH and L_Edd are, respectively, the viscosityparameter, gas accretion rate onto the central black hole (BH), the BH mass andthe Eddington luminosity). Moreover, lsg is as small as 1500 AA for alpha =0.001, which is the smallest alpha case in this study. Therefore, the windowfor observing the self-gravitating part of an AGN accretion disc is from 2micron to lsg. Incidentally, rsg can be less than the photon trapping radiusfor Mdot >~ 10^3.3 L_Edd/c^2. Namely, a self-gravitating, optically-thick,advection-dominated accretion disc is expected to appear in the extremely highaccretion rate regime.  Next, we demonstrate that the Mid-Infrared to X-ray spectrum of a bright,well-studied Narrow-Line Seyfert 1 galaxy, Ton S 180, is indeed well fitted bythe spectrum arising from the following three components: an inner slim disc(with a corona), an outer, self-gravitating non-Keplerian disc and a dustytorus. The total mass, BH mass plus the entire disc mass, is found to be about(1.4 - 8.0) M_BH. If the surface density varies with radius r in proportion tor^-0.6, the total mass is consistent with the central mass estimated by H_betaand [O III] widths.Comment: 8 pages (including 5 figures), Latex, Accepted for publication in  Astronomy and Astrophysic

The origin of optical emission from super-Eddington accreting Active Galactic Nuclei: The case of Ton S 180