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

Astrophysics, abstract
astro-ph/0304085

From: Hujeirat <hujeirat@mpia-hd.mpg.de>

Date: Thu, 3 Apr 2003 22:56:14 GMT   (468kb)

Authors:
A. Hujeirat

Based on theoretical arguments and quasi-stationary radiative MHD
calculations, a model for accretion-induced jet is presented. It is argued that
accretion disks around BHs consist of 1) a cold, Keplerian-rotating and weakly
magnetized medium in the outer part, 2) highly advective and turbulent-free
plasma inside $r_mm{tr} = 10-20$ Schwarzschild radii, where magnetic fields
(-MFs) are pre-dominantly of large scale topology, and in excess of thermal
equipartition, and 3) an ion-dominated torus in the vicinity of the hole, where
MFs undergo a topological change into amonopole like-topology. The action of
MFs interior to $r_mm{tr}$ is to initiate torsional Alfven waves (-TAWs) that
extract angular momentum from disk-plasma and deposit it into the transition
layer (-TL) above the between the disk, where the plasma is dissipative and
tenuous. A significant fraction of the toroidal magnetic field (-TMF) reconnect
in the TL, thereby virial-heating the ions and forming a two-temperature,
super-Keplerian rotating, centrifugal-accelerated ion-dominated outflows. The
TMF in the TL is in thermal equipartition with the ions, whereas the poloidal
component (-PMF) is with the electrons. Such a strong TMF is essential for
increasing the jet-disk luminosity in the radio regime.

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