A model for electromagnetic extraction of rotational energy and formation of accretion-powered jets in radio galaxies*
Max-Planck-Institut für Astronomie, 69117 Heidelberg, Germany
Corresponding author: email@example.com
Accepted: 21 November 2003
A self-similar solution for the 3D axi-symmetric radiative MHD equations is presented, which revisits the formation and acceleration of accretion-powered jets in AGNs and microquasars. The model relies primarily on electromagnetic extraction of rotational energy from the disk plasma and forming a geometrically thin super-Keplerian layer between the disk and the overlying corona. The outflowing plasma in this layer is dissipative, two-temperature, virial-hot, advective and electron-proton dominated. The innermost part of the disk in this model is turbulent-free, sub-Keplerian rotating and advective-dominated. This part ceases to radiate as a standard disk, and most of the accretion energy is converted into magnetic and kinetic energies that go into powering the jet. The corresponding luminosities of these turbulent-truncated disks are discussed. In the case of a spinning black hole accreting at low accretion rates, the Blandford-Znajek process is found to modify the total power of the jet, depending on the accretion rate.
Key words: galaxies: jets / black hole physics / accretion, accretion disks / magnetohydrodynamics / radiative transfer
© ESO, 2004