The power of the jets accelerated by the coronal magnetic field

Abstract

It was suggested that the large scale magnetic field can be dragged inwards efficiently by the corona above the disc, i.e., the so called "coronal mechanism" (Beckwith, Hawley, \& Krolik 2009), which provides a way to solve the difficulty of field advection in a geometrically thin accretion disc. In this case, the magnetic pressure should be lower than the gas pressure in the corona. We estimate the maximal power of the jets accelerated by the magnetic field advected by the corona. The Blandford-Payne (BP) jet power is found always to be higher than the Blandford-Znajek (BZ) jet power, except for a rapidly spinning black hole with a>0.8. The maximal jet power is always low, less than 0.05 Eddington luminosity, even for an extreme Kerr black hole, which is insufficient for the observed strong jets in some blazars with jet power $\sim 0.1-1$ Eddington luminosity (or even higher). It implies that these powerful jets cannot be accelerated by the coronal field. We suggest that, the magnetic field dragged inward by the accretion disc with magnetically outflows may accelerate the jets (at least for the most powerful jets, if not all) in the blazars.

4 pages, accepted by MNRAS, references updated

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• The large-scale magnetic field advected in the corona of a thin accretion disk
• General Physical Properties of Gamma-Ray-emitting Radio Galaxies
• The dynamical structure of the outflows driven by a large-scale magnetic field
• The Accretion Properties and Jet Mechanisms for the Low-Excitation Radio Galaxies