Magnetized thin accretion disks in active galactic nuclei - A quantitative analysis of field topologies and their dynamic importance

Details Magnetized thin accretion disks in active galactic nuclei - A quantitative analysis of field topologies and their dynamic importance Magnetized thin accretion disks in active galactic nuclei - A quantitative analysis of field topologies and their dynamic importance

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...263..401k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 263, no. 1-2, p. 401-412.

Statistics

Computation

16

Accretion Disks, Active Galactic Nuclei, Black Holes (Astronomy), Interstellar Magnetic Fields, Magnetic Field Configurations, Topology, Angular Momentum, Computational Astrophysics, Dynamo Theory, Field Strength, Turbulence Effects

Scientific paper

Stationary solutions of the MHD induction equation are presented for a thin accretion disk surrounding a black hole of 10 exp 9 solar masses. A radially dependent magnetic diffusivity is assumed in accounting for disk plasma turbulence. A fast centrifugally driven jet which is almost force-free close to the disk can be produced in principle in dipolar field topology. A jet driven by a disk with quadrupolar field topology is slower and not force-free at its foot point. The dipolar fields get strong enough to contribute up to 50 percent of the torque required for angular momentum transport in the innermost region. In the outer parts of the disk magnetic tensions cause an effect of only a few percent. Poynting flux from a magnetized disk can heat a corona and inject magnetic energy into jets. For even Psi symmetry the transported magnetic power is about five times the accretion luminosity of an AGN with a 10 exp 9 solar mass central black hole and a moderate accretion rate of 1 solar mass/yr.

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