Jet-formation in accreting black hole systems and in GRB

Abstract

Most powerful jets are observed to emanate from accreting black hole systems. Recent quasi-stationary radiative MHD calculations reveal that jet-launching start in the innermost region of a transition layer (:TL), which is located between the disk and the corona. The plasma in the TL is dominated by virial-hot protons, advective, highly magnetic-diffusive and rotates super-Keplerian. The amplified toroidal magnetic field (TMF) in the TL reach values beyond equipartition with respect to the electron thermal energy, thereby considerably enhancing the Poynting energy flux and yielding gravitationally unbound electron-proton outflows with a positive Bernoulli number. We speculate that beaming jets in GRBs may possess similar properties, provided that the GRB-progenitors have rotational energy sufficient for forming a nearly Keplerian and massive disk.