
TY  - JOUR
A1  - Donea, Alina-C. 
A1  - Biermann, Peter L. 
T1  - The Structure of Accretion Flow at the Base of Hets in AGN
JF  - Publications of the Astronomical Society of Australia
JO  - Publ. Astron. Soc.  Aust.
Y1  - 2002
VL  - 19
IS  - 1
SP  - 125
EP  - 128
KW  - accretion, accretion disks &#8212; galaxies: jets &#8212; galaxies: active &#8212; galaxies: nuclei
UR  - https://doi.org/10.1071/AS01078 
N2  - This paper discusses the boundary layer and the emission spectrum from an accretion disk having a jet anchored at its inner radius, close to the black hole. We summarise our earlier work and apply it to the accretion disks of some blazars. We suggest that the &#8216;accretion disk with jet&#8217; (ADJ) model could make the bridge between standard accretion disk models (suitable for quasars and FRii sources) and low-power advection dominated accretion disk models (suitable for some of the low-power BL Lacs and FRi sources). The jet is collimated within a very narrow region close to the black hole (nozzle). In our model it is assumed that the boundary layer of the disk is the region between radius Rms &#8212; the last marginally stable circular orbit calculated for a Kerr geometry &#8212; and the radius Rjet, which gives the thickness of the &#8216;footring&#8217;, i.e. the base of the jet. We analyse the size of the boundary layer of the disk where the jet is fed with energy, mass, and angular momentum. As a consequence of the angular momentum extraction, the accretion disk beyond Rjet no longer has a Keplerian flow. A hot corona usually surrounds the disk, and entrainment of the corona along the flow could also be important for the energy and mass budget of the jet. We assume that the gravitational energy available at the footring of the jet goes into the jet, and so the spectrum from the accretion disk gives a total luminosity smaller than that of a &#8216;standard&#8217; accretion disk, and our ADJ model should apply for blazars with low central luminosities. Variations of the boundary layer and nozzle may account for some of the variability observed in active galactic nuclei. 
ER  -

