C.D.S. - SIMBAD4 rel 1.7 - 2021.04.19CEST13:23:32

2003A&A...408..415H - Astronomy and Astrophysics, volume 408, 415-430 (2003/9-3)

A model for the jet-disk connection in BH accreting systems.


Abstract (from CDS):

The powerful and highly collimated jets observed in active galactic nuclei and µ-quasars are likely to be connected to the accretion phenomenon via disks. Based on theoretical arguments and quasi-stationary radiative MHD calculations, a model for an accretion-powered jet is presented. It is argued that accretion disks around black holes consist of 1) a cold, Keplerian-rotating and weakly magnetized medium in the outer part, 2) a highly advective and turbulent-free plasma inside rtr=10-20 Schwarzschild radii, where magnetic fields are predominantly of large scale topology and in excess of thermal equipartition, and 3) an ion-dominated torus in the vicinity of the hole, where magnetic fields undergo a topological change into a monopole like-configuration. The action of magnetic fields interior to rtr is to initiate torsional Alfven waves that extract angular momentum from the disk-plasma and deposit it into the transition layer between the disk and the overlying corona, where the plasma is dissipative and tenuous. A significant fraction of the shear-generated toroidal magnetic field reconnects in the transition layer, thereby heating the plasma up to the virial-temperature and forming a super-Keplerian rotating, and hence centrifugally accelerated outflow. The strong magnetic field in the transition layer forces the electrons to cool rapidly which, in combination with the fast outward-oriented motion, yields a two-temperature ion-dominated outflow. The toroidal magnetic field in the transition layer is in thermal equipartition with the ions, whereas the poloidal component is in equipartition with the electrons. Such a strong toroidal magnetic field is essential for increasing the jet-disk luminosity in the radio regime. These gravitationally unbound outflows serve as seeds, possibly, for all the powerful electron-proton jets observed in accreting systems containing black holes.

Abstract Copyright:

Journal keyword(s): methods: N-body simulations - galaxies: jets - black hole physics - accretion, accretion disks - magnetohydrodynamics - radiative transfer

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1400 0
2 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
3 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1751 1
4 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2361 0
5 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3997 0

    Equat.    Gal    SGal    Ecl

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