Computer Science
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..374b&link_type=abstract
MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp
Computer Science
Accretion Disks, Magnetic Fields, Galactic Nuclei, Black Holes, Magnetohydrodynamics And Plasmas, Galactic Nuclei, Circumnuclear Matter, And Bulges, Black Holes
Scientific paper
We summarize the main features of an accretion disk model that incorporates the effect of a turbulent magnetic field, ab initio and which also considers the dynamics of the disk-wind-corona system. The vertical-azimuthal magnetic stress can be important for both angular momentum transport and energy when it is of order 1% of the usual radial-azimuthal flux. The Poynting flux associated with the product of this additional stress with the Keplerian velocity is also likely to be the dominant component of the Poynting flux from the disk in to the corona. Suitably evolved estimates of magnetic fields in accretion disks are compared with estimates in blazars with some interesting differences. The resolution of these differences should be informative, both for blazar and accretion disk models. Further evolution of the magnetic field from the TeV-emitting scale to the VLBI scale in the blazars MKN 421 and MKN 501 is consistent with the notion that the jets in those sources decelerate from highly relativistic to mildly relativistic velocities.
Bicknell Geoffrey V.
Kuncic Zdenka
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